VarS
SITI — Variab
bility off the Sunn and Itts Terreestrial Impact
I

Seecondd VarrSITII Gen
nerall Sym
mposiium

ABS
STRA
ACTS
S

I
Irkutskk, Russsia, 10
0–15 Juuly 20117

Scientific Organizing Committee:
VarSITI Co-Chairs:
Kazuo Shiokawa (Japan)

Katya Georgieva (Bulgaria)

Members:
Nat Gopalswamy (USA)Jacob Bortnik (USA)
Geliy Zherebtsov (Russia)
Shrikanth Kanekal (USA)Petra Knizova (Czech Republic)
Andrey Medvedev (Russia)
Alexei Krivolutsky (Russia)
Vladimir Kuznetsov (Russia)
Franz–Josef Lübken (Germany)
Petrus Martens (USA)
Yoshizumi Miyoshi (Japan)

Valery Nakariakov (UK)
Igor Mokhov (Russia)
Vladimir Obridko (Russia)
Dibyendu Nandi (India)
Anatoly Petrukovich (Russia)
Takashi Watanabe (Japan)
Craig Rodger (New Zealand)
Annika Seppälä (Finland)
Manuela Temmer (Austria)
William Ward (Canada)
Jie Zhang (USA)

Local Organizing Committee:
Vladimir Kurkin (Chair)
Robert Sych (Co-Chair)
Larisa Kashapova
Ekaterina Korzhova
Dmitry Klimushkin
Konstantin Ratovsky
Irina Medvedeva
Ilya Edemskiy
Dmitry Andryashin
Marina Nikonova

Sponsors:
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ROSTEC Corporation (ROSTEC)
Variability of the Sun and Its Terrestrial Impact (VarSITI/ SCOSTEP)
Russian Fund for Basic Research (RFBR)
Federal Agency for Scientific Organizations (FASO)
Institute for Space-Earth Environmental Research (ISEE)National Science Foundations (NSF)
Committee on Space Research (COSPAR)
Project for Solar-Terrestrial Environment Prediction (PSTEP)PWING project (PWING)
The Japan Society for the Promotion of Science (JSPS)

Second VarSITI General Symposium (VarSITI-2017) was held with the financial support
from the Russian Foundation for Basic Research, Project No. 17-05-20306.

Session 1: SOLAR AND HELIOSPHERIC DRIVERSOF EARTH-AFFECTING EVENTS_____________________________________________________________WAVE DYNAMICS IN UMBRAL FLASHES
Robert Sych1, Wang Min2, Zhong Liu2
12

Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
Yunnan Astronomical Observatory, Chinese Academy of Sciences, Kunming, China

sych@iszf.irk.ru

We study the spatial distribution of oscillation sources EUV emission in different temperaturechannels SDO/AIA above sunspot umbra. For the first time the high-resolution imaging are
employed to study the wave processes in magnetic structures with different spatial and heights scales,connected with short-term energy release as an umbra flashes (UFs). We used the pixelized wavelet
filtration (PWF-analysis) for obtain temporal dynamic of waves as well as prepared the space-time
diagrams. It is shown that UFs sources mainly localized near the footpoints of magnetic loops along
which waves propagated with 3 min periodicity. We find two types of the UFs sources - pointed andextended. The first type of sources connected with the footpoints of open field lines, the second withclosed lines. Temporal dynamics of flashes shows the increasing of three-minute oscillations before
UFs peak within low-frequency wave train. It is shown that the maximum oscillations trains coincidewith the peak intensity of umbral flashes. Fine spatial structure of magnetic waveguides during
UFs was observed. It is shown that UFs are short-term wave activity at footpoints of selected coronalloops, rooted in the sunspot umbra. We suggested that depending from the inclination angle ofmagnetic tubes to the solar normal there are various modes of propagating waves. This relationshipdefines the UFs lifetime, their power, and angular size of the sources.
A STUDY OF TROPICAL CYCLONES OVER INDIA (BAY OF BENGAL
AND ARABIAN SEA) AND SOLAR INFLUENCE ON IT
Dhruba Banerjee
Faculty Member, Swami Vivekananda Institute of Science and Technology, Dakshin Gobindapur,
Kolkata-700145, India
dhrubabanerjee81@gmail.com

A prominent example of extreme weather event in India is cyclonic storm. In this paper
annual variation of tropical cyclonic storm (CS), severe cyclonic storm (SCS), very severe
cyclonic storm (VSCS) and super cyclonic storm (SuCS) over Bay of Bengal (BOB) andArabian Sea (ARS) during last 20 years (1990–2009) have been analyzed. The analysis revels
that the total number of cyclone (TNC) has increased with high rate (gradient being +1.67 peryear) and although CS is more over BOB than that over ARS. The rate of increase of CS overArabian Sea is more than that over Bay of Bengal. Furthermore, two interesting features havebeen noted: (i) Monsoon tends to prohibit the formation of CS; (ii) cyclonic storm (CS) increases
with the increase of global sea surface temperature (GSST) during said period. Attempt has also
been made to find out the influence of solar activity on these extreme weather events. Keeping in
mind that the Sun Spot Number (SSN) is an indicator of the strength of solar effects, it has been3

found that in most of the times the high value of SSN is associated with small number of total
cyclone (CS). Specifically, when only the years of high Suns spot number (approximately greaterthan 90) are taken into consideration then correlation coefficient (CC) between SSN and numberof cyclones comes out to be quite high (–0.78) significance at 99.99.
ON THE MECHANISM OF PARTICLE ACCELERATION IN SPACE
Igor Podgorny1, Alexander Podgorny2
12

Institute of Astronomy RAS, Moscow, Russia
Lebedev Physical Institute RAS, Moscow, Russia

podgorny@inasan.ru

The possibility of particle acceleration in space is considered in dozens of books. All theseworks are based on unproven assumptions that cannot be confirmed by long-term observations.
The solar cosmic rays discovery and the information received from the measurements with theworldwide network of neutron monitors and with spacecraft beyond the Earth’s magnetic field
allow us to conclude that the solar cosmic rays are accelerated in solar flares. It is shown that theobserved spectra of protons are created due to current sheet decay. These phenomena are welldescribed by the electrodynamical solar flare model built on the basis of observational data andnumerical MHD simulations using the initial and boundary conditions taken from observationsof active regions before the flare. The main factor determining the formation of the solar cosmic
ray pulses recorded near the Earth is the interplanetary magnetic field. The undistorted spectrumof accelerated protons arriving to Earth is observed only in the front of a proton pulse of theflares that have occurred in the western part of the solar disk. These particles come without
collisions along the magnetic field lines of the Archimedes spiral. However, the distribution of
protons recorded with delay has a diffusion character indicating the development of the beam
instability. New information about the solar cosmic rays puts forward the important question:
can the mechanism of acceleration of solar flare protons explain the acceleration of the particles
of galactic cosmic rays. The problem of the solar cosmic ray prediction is also not solved.
FLARE POSITIONS FOUNDED FROM MHD SIMULATION RESULTS AND X-RAY
SOURCES ABOVE THE ACTIVE REGION 10365
Alexander Podgorny1, Igor Podgorny2, Natalia Meshalkina3
1

Lebedev Physical Institute RAS, Moscow, Russia
Institute of Astronomy RAS, Moscow, Russia
3
Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
2

podgorny@lebedev.ru

Numerical MHD simulation demonstrates the current sheet creation in the solar corona
above an active region before the flare. Solar flare appearance and its observational
manifestations can be explained by fast release of the energy stored in the current sheet magnetic
field when the current sheet transforms into an unstable state. Intensive magnetic fielddissipation causes plasma heating and therefore the appearance of the thermal X-ray emission
source. The magnetic field configuration in the corona cannot be obtained from the observations.
The magnetic field configuration in the corona is found by numerical solving of MHD equations
using the observed magnetic field distribution on the photosphere for setting boundary4

conditions. The finite-difference scheme which is stable for large steps is developed to acceleratecalculation. This scheme is upwind, absolutely implicit, and it is conservative relative to themagnetic flux. The graphical method for search the flare position and study of magnetic field inthe solar corona has been developed. This method uses the property of the current sheet,according to which the local maximum of the current density is located in the center of a current
sheet. The results of numerical simulation of flares May 27, 2003 at 02:53 and May 29, 2003 at
00:51 permit to conclude that the current sheet position coincides with the position of the thermal
X-ray sourсe. The RHESSI measurements are used. The magnetic field configuration near thecurrent sheet in the corona above the active region 10365 for flares May 27, 2003 at 02:53 andMay 29, 2003 at 00:51 shows that the physical meaning of the processes of accumulation andrapid energy release of the flare are demonstrated by the lines that perpendicular to the force
vectors. These lines are located in the current sheet configuration plane.
MULTIFRACTAL DETRENDED FLUCTUATION ANALYSIS OF SOLAR WIND
PLASMA AND INTERPLANETARY MAGNETIC FIELD DURING GEOMAGNETIC
STORMS
Deepak Kumar Sondhiya
Department Of Physics, Barkatullah University, Bhopal, India
deepsondhiya@gmail.com

We have analyzed the data of solar plasma parameters and interplanetary magnetic field
during intense geomagnetic storms. The analysis for solar wind plasma and interplanetary
magnetic field is very importance for the better understanding of various phenomena in theenvironment of sun and its connection with the space weather conditions. For this purpose
wavelet based advanced multifractal detrended fluctuation analysis (MFDFA) method was usedin this work. The behavior of solar plasma parameter and interplanetary magnetic field arequantitatively described by the Scaling Function, Hurst exponent, Mass exponent andmultifractal spectrum. This method derives the phenomena of intermittence in data during
intense geomagnetic storms and also provides some interesting deterministic and chaotic features.
The results of analysis gives the confirmation of non-uniform nature of solar plasma turbulence
which driving the plasma emission process and its connection with the interplanetary magnetic field.
FLARING ENERGY RELEASE AND PARTICLE ACCELERATION
IN THE LOWER SOLAR ATMOSPHERE
Alexander Stepanov1, Valery Zaitsev2
1
2

Pulkovo Observatory, Saint Petersburg, Russia
Institute of Applied Physics, Nizhny Novgorod, Russia

stepanov@gao.spb.ru

New challenges to the standard model of solar flares motivated by modern observations
with the spacecraft and ground-based telescopes are presented. The most important are in situ
heating of chromospheric loop footpoints up to the coronal temperatures without precipitating
particle beams from the corona, and the sunquakes which are unlikely to be explained by the
impact of energetic particles producing hard X-ray emission. The long-standing ‘number
problem’ in the physics of solar flares is also unresolved problem. It is shown that modern
observations favored an important role of the electric currents in the energy release processes in the
low solar atmosphere. Particle acceleration mechanism in the electric fields driven by the magnetic
5

Rayleigh-Taylor instability in the chromosphere is proposed. The electric currents I ≥ 1010 A, needed
for the excitation of super-Dreicer electric fields in the chromosphere are determined. It is shown thatboth Joule dissipation of the electric currents and the particles accelerated in the chromosphere canbe responsible for in situ heating of the low solar atmosphere. The Alfven-Carlqvist model of thesolar flare based on the electric circuit approach is developed. Interaction of a current-carrying loopwith the partially-ionized plasma of prominence in the context of particle acceleration is considered.
The role of sub-THz and THz emission in the study of flaring activity is discussed.
EARTH-AFFECTING CMEs AND ASSOCIATED GEOMAGNETIC STORMS
Yuming Wang, Chenglong Shen, Yutian Chi
University of Science and Technology of China, China
ymwang@ustc.edu.cn

Initially Earth-directed coronal mass ejections (CMEs), which usually look like a halofrom the Earth, are believed to be the most probable candidates of Earth-affecting CMEs.
However, not all of initially Earth-directed CMEs can encounter the Earth, and moreover, not allof Earth-encountered CMEs can cause a geomagnetic storm. In this talk, starting from a sample
of full halo CMEs during 1997 March – 2012 May, we show that (1) even for full halo CMEs,
they were not necessary to propagate along the Sun—Earth line; the deviation angle could belarger than 45 degrees, (2) the apparent speed observed in a coronagraph may differ largely fromthe true value for the CMEs propagating within 45 degrees of the Sun-Earth line and slower than
900 km/s, (3) the deflection and interaction of CMEs in interplanetary space may further
influence the possibility of a CME encountering the Earth as well as their Earth-arrival time.
Further, by investigating the ICMEs and Dst index from 1995 to 2015, we show the statisticalproperties of these Earth-encountered CMEs and their capability in causing geomagnetic storms.
Although isolated CMEs are the major source of geomagnetic storms, shock-CME interacting
structures demonstrate an increasing role in causing stronger geomagnetic storms.
QUIESCENT FILAMENT ERUPTION AND ASSOCIATED FLARE
ON 29 SEPTEMBER 2013
Ramesh Chandra
Kumaun University, Nainital, Indiarchandra.ntl@gmal.com

We present here the evolution of a quiescent filament during 26 August to 29 September,2013. For the evolution of filament we have used the data from Solar Dynamics Observatory(SDO), STEREO and GONG H-alpha. After the survival of nearly one month, it was erupted on
29 September, 2013 around 21:15. The eruption was associated with GOES C 1.6 flare, coronalmass ejection (CME), and type II radio bursts. The Kinematics of filament eruption and CME isalso discussed here. In order to discuss the magnetic causes of filament eruption, we have used
the magnetic field data from HMI onboard SDO satellite. We have observed the magnetic flux
cancellation at filament’s footpoints, which could be possible reason for its eruption. Finally, we
have interpreted our observations in light of eruption models.

6

GEOEFFECTIVENESS OF SIRs FROM 1995 TO 2015
Chenglong Shen
School of Earth and Space Sciences, University of Science and Technology of China, Hefei, Anhui,
230026, China
clshen@ustc.edu.cn

Stream Interaction Region (SIR) which is caused by the interaction between a fast solar
wind stream and a slow solar wind stream ahead of it. SIRs are thought to be a main source ofthe minor geomagnetic storm especially in the declining phase and around solar minimum. In
this paper, we extend the time period of Jian Lan’s SIR catalog, which cover the time range from1995 to 2009, to the end of 2015. In this catalog, we have totally 37 SIR events. Studied the Dst
index from WDC geomagnetic index center, we found that 54.4 % (401) of SIR events caused
geomagnetic storms with Dstmin< – 30 nT, while 3.3% (24) of SIR events caused intense
geomagnetic storms with Dstmin< – 100 nT. Meanwhile, for all SIR events, we find 186 (25.2 %)SIR events contain little flux rope. We compare the geoeggectiveness of SIRs with flux ropes
and SIRs without flux rope, and find that the percentage of SIR with flux rope events caused
intense geomagnetic storm is higher than that of SIR without flux rope. In addition, we also
compare the geoeffectiveness of SIRs in solar cycle 23 and solar cycle 24.

THERMAL INSTABILITY OF CURRENT LAYER AS A TRIGGERFOR SOLAR FLARES
Leonid Ledentsov, Boris Somov
Sternberg Astronomical Institute, Moscow State University, Moscow, Russia
koob@mail.ru

The modern satellite observations of flare arcades in solar flares demonstrate a consistentincrease in the brightness of individual coronal loops. We have solved the problem of the small
perturbations stability of a homogeneous longitudinal reconnecting current layer in the MHD
approximation. The suppression of the plasma thermal conductivity by the magnetic field inside
the current layer provides an instability. The instability increases in a radiative cooling time scaleof the plasma in the linear phase. A periodic structure of hot and cold fibers arrangedtransversely to the direction of the electric current are formed as a result of the instability. The
proposed mechanism of the thermal instability can be useful for an explanation of the consistentincrease in the brightness of individual coronal loops in solar flares.

7

PHOTOSPHERIC MAGNETIC FIELD VARIATIONS DURING THE 7 JUNE 2011 M2.5
FLARE
Yaroslav Egorov, Victor Fainshtein, George Rudenko
Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
egorov@iszf.irk.ru

From the vector measurements of the photospheric magnetic field with the SDO/HMI
instrument, we study the field variations within the 2011 June 7 eruptive event related to afilament eruption, flare, and coronal mass ejection. Analyzed were the variations in the magnetic
strength modulus (B), radial (Br), and transversal (Bt) a component, as well as field line
inclination (α) to the radial direction from the Sun center. The field line time variations withindifferent sites of the eruptive event were studied in detail. The field line inclination was revealed
to decrease in its channel surroundings during the filament slow emergence, whereas, in the flareregion, near the magnetic polarity inversion line (PIL), the inclination angles (α) dramaticallyincrease after the flare onset. Besides, in the flare region, after its onset, the magnetic strength
magnitude and its transversal component increase. Diverging flare ribbons are shown to belocated over the photosphere regions with the field modulus local maxima and with deep minimaof the field line inclination. Near PIL, the photospheric magnetic field azimuth decreases after
the flare onset, which implies a decrease in angle α between PIL and the magnetic strength
vector projection onto the sky plane, or, in other words, the shear increase. Far from PIL, on thecontrary, the azimuth increases, and, correspondingly, the angle α also increases. The magnetic
field gradient averaged separately in the field with positive and negative polarity in the domain,
where B, Bt, and α increase, dramatically decreases starting with the GOES peak X-ray flux.
VARIATIONS IN THE CHARACTERISTICS OF THE SUNSPOT UMBRA MAGNETIC
FIELD DURING FLARES AND CORONAL MASS EJECTIONSYuliya Zagainova1, Victor Fainshtein2, George Rudenko2, Vladimir Obridko1
1

Pushkov Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation RAS,
Moscow, Russia
2
Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
yuliazag@izmiran.ru

Geometrical and physical properties of sunspots may vary during eruptive events (afilament eruption, a flare, a CME). Sunspot penumbra time variations have been studied most
scrupulously by now. At the same time, there is scarce information on the sunspot umbra
property variations accompanying eruptive events. Knowing regularities of such variations
before the eruptive event onset may be used to predict eruptive events. We studied variations inthe sunspot umbra magnetic field characteristics of active regions (ARs), where there were
eruptive events of 2011 August 2, 2012, March 9, 2013, April 4, 2014, January 7, and June 18,
2015. We analyzed the behavior of the magnetic strength modulus maximum Bmax, the magnetic
field line minimal inclination angle to the radial direction from the Sun center αmin (i.e., themagnetic tube inclination angle from the sunspot umbra), and also the mean (within the umbra)
values <B> and <α>. It is shown a change in the above magnetic field parameter behavior isshown to occur after the flare onset as compared with those observed before the flare onset (e.g.,8increase/decrease in the parameter before the flare onset gives way to its decrease/increase or aweak variation after the flare onset). But the variation view is different in different spots of ARs.
In some cases, Bmax and <B> vary in correlation after the flare onset; in other cases, they vary inantiphase. One may arrive at a similar conclusion relative to the time variations in αmin and <α>.
We revealed that an essential variation in the umbra magnetic properties was observed in thesunspot located near one of the magnetic loop feet, whose motion leads to forming a CME
frontal structure. We discovered that, within ≈3 hours before the flare onset, a decrease in the
αmin was observed, with ≈ 10° to ≈ 4°, with its subsequent (after the flare onset), rapid decrease
to small values (≤1°) over ≈30 min. Simultaneously, the angle <α> varied (decreased)significantly more weakly. This means that, after the flare onset, the magnetic tube from theumbra of such sunspots diverges from its initial position almost as a whole, i.e., without essential
transformation of the magnetic field line distribution inside the tube. As to the magnetic fieldmagnitude, Bmax and <B> increase by about 200 G within 2 hours after the flare onset.

COMPARISON BETWEEN MAGNETIC PROPERTIES AND UMBRA AREA OFWESTERN AND EASTERN SUNSPOTS WITH DIFFERENT ASYMMETRY OF THE
CONNECTING MAGNETIC FIELD
Yuliya Zagainova1, Victor Fainshtein2, George Rudenko2, Vladimir Obridko1
1

Pushkov Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation RAS,
Moscow, Russia
2
Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
yuliazag@izmiran.ru

We compared magnetic properties (maximum Bmax and mean value <B> of the magnetic
strength, the inclination angle of the magnetic tube to the radial direction from the Sun center
αmin, and the mean inclination angle of the field lines <α>), and also these characteristics andthe umbra area S separately for the umbra of western and eastern sunspots with asymmetry of themagnetic field tying connecting them. The asymmetry character is determined by the ratio
between the magnetic tube inclination angles in two types of sunspots (western/eastern). For theselected group of the magnetically-connected sunspots (i.e., the sunspots connected by field lines
calculated in potential approximation) recorded over 2010–2014, the inclination angle of themagnetic tube from the western sunspot umbra is shown to be smaller than the analogous angle
from the eastern sunspot umbra in 70 % of the addressed sunspot pairs. We revealed that suchdependences, like αmin(S) and Bmax(S), feature equal trends, and are quantitatively close forsunspot groups with different asymmetry of the magnetic field tying connecting them. At thesame time, the connection <α> with S and with <B> in the sunspot umbra appeared different for
two sunspot groups. We studied the position of the polarity inversion line of the photosphericmagnetic field radial component relative to the magnetically-connected western and easternsunspots. We draw a conclusion that, in ≈ 54–74 % of cases (depending on the character of
averaging the field radial component distribution), the field polarity inversion line is closer to thewestern sunspot. Also, in most of these cases, the inclination angle of the magnetic tube from thewestern sunspot umbra is less, than the analogous angle from the eastern sunspot umbra. These
results allow us to doubt the earlier conclusion that all the magnetically-connected sunspots areformed due to the emergence of a magnetic loop from the convection zone depth. Indeed, from9

calculations of such tube emergence, due to the Coriolis force effect, the inclination angle of the
tube from the eastern sunspot umbra should be less than the inclination from the western sunspot
umbra, which does not agree with observations for a large group of the magnetically-connected
western/eastern sunspots.
ON THE REDUCED GEOEFFECTIVENESS OF SOLAR CYCLE 24: A MODERATESTORM PERSPECTIVE
Selvakumaran Ravindran1, Veenadhari Bhaskara1, Sachiko Akiyama2, Megha Pandya1,
Gopalswamy Nat2, Sandeep Kumar1, Seiji Yashiro2, Pertti Mäkelä2, Hong Xie2
1
2

Indian Institute of Geomagnetism, Mumbai, Maharashtra, India
NASA Goddard Space Flight Center, United Statesselva2986@gmail.com

The moderate and intense geomagnetic storms are identified for the first 77 months of solar
cycle 23 and 24. The solar sources responsible for the moderate geomagnetic storms areindentified during the same epoch for both the cycles. Solar cycle 24 has shown nearly 80 %reduction in the occurrence of intense storms where as it is only 40 % in case of moderate storms
when compared to previous cycle. The solar and interplanetary characteristics of the moderate
storms driven by CME are compared for solar cycle 23 and 24 in order to see reduction in
geoeffectiveness has anything to do with the occurrence of moderate storm. Though there is
reduction in the occurrence of moderate storms, the Dst distribution does not show muchdifference. Similarly the solar source parameters like CME speed, mass and width did not show
any significant variation in the average values as well as the distribution. The correlation
between V Bz and Dst is determined and it is found to be moderate with value of 0.68 for cycle
23 and 0.61 for cycle 24. These results are significantly different when total geomagnetic storms
are taken in to consideration for both the solar cycles.
CME-RELATED SHOCK GENERATION WITHIN THE LASCO C3 CORONAGRAPH
FIELD-OF-VIEW
Victor Fainshtein, Yaroslav Egorov
Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
vfain@iszf.irk.ru

CME-related shocks play an important role in space weather, and, in many cases,
determine characteristics of geomagnetic disturbances when shocks impact the Earthmagnetosphere. The shock properties in the Earth orbit largely depend on peculiarities of theirgeneration on the Sun. There are two viewpoints concerning the nature of CME-related shocks
observed within the LASCO C2, C3 coronagraph fields. According to one viewpoint, all suchshocks are piston, with a CME body as a piston, but there was no information on where suchshocks originated for the bulk of the analyzed events. According to the other viewpoint, at least,a part of such shocks are generated in the lower corona by an eruptive filament rapidly
accelerated to relatively high velocities, or by a flux rope disturbing the ambient corona. Rightafter its origin, this wave propagates as an explosive one, and, at a sufficient distance from its
origin, it may start to behave as piston. We are the first to investigate the CME-related shock10

generation within the LASCO C3 coronagraph field-of-view, i.e., at relatively large distances.
Addressed was CME recorded, for the first time, within the LASCO C2 field on 2012 July 17(13:48 UT). Peculiarities of the addressed CME are its forming at a relatively significant height,
and the CME body slow acceleration with distance. The shock originated at a distance surpassing
12 solar radii, when the CMA body velocity exceeded the total velocity Va+Vsw, where Va is the
Alfvenic velocity, Vsw is the solar wind velocity on the CME body axis. Based on this, there
came a conclusion that the formed shock is a bow shock, and it was generated, when the ambient
plasma flowed around the CME body at a super-Alfvenic speed. The generated shock appears
collisionless, because its front width is many fold less than the coronal plasma charged particle
free path. We came to a conclusion that the oft-used distance dependence Va from (Mann et al.,1999) is incorrect, and provides the underrated values. Therefore, we found an Alfvenic velocity
distance dependence by using representative values of the magnetic field radial component, theproton concentration in the Earth orbit, and the known regularities of the distance variation in
those solar wind characteristics separately in the fast and slow solar wind. Because the CME
body axis appeared, by estimates, in the slow wind domain, we used the slow solar wind velocity
from Sheeley N.R.,Jr. et al. (1997) as Vsw velocity. For several instants, we found a brightness
jump at the front of the generated shock and the Alfvenic Mach number. Compared were thevariations in the shock velocity and in the CME body velocity.

KINEMATICS OF CMEs AND RELATED SHOCKS FROM LASCO DATA:COMPARATIVE ANALYSIS
Victor Fainshtein1, Yaroslav Egorov1, Yuliya Zagainova2
1

Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
Pushkov Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation RAS,
Moscow, Russia
2

vfain@iszf.irk.ru

For two groups of fast CMEs related to a shock within the LASCO field, we determined
time dependences for the boundary positions of the CME body and of the shock, as well as thevelocities of these structures. Separately, we analyzed limb CMEs, whose sources were locatedwithin 30o relative to the limb, and a halo CME (HCME) with sources within 30o relative to thesolar disk center. In the former case, the kinematics of the CME and the shock within the
LASCO С2 and С3 field reflects the result of the joint effect of the CME translational motion
CME and its expansion. In the latter case, the peculiarities of the CME and shock motions are
determined, preferentially, by the expansion of these structures. These results were compared tothe time dependences of the CME and shock kinematic parameters in 3D. The kinematicparameters were determined by using the «Ice cream cone model» for a mass ejection. On
average, the shock velocity was shown to be higher than that of the CME body in all the cases
practically to the boundary of the LASCO C3 field. But the character of the variation in the CME
body velocity and in the shock velocity differs both for each CME group, and in comparison
between different CME groups. On average, both the CME velocity and the shock velocity
decreases with time (distance) for the limb and halo CMEs from observations within the LASCO
С2 and С3 field. And for both CME groups, the shock velocity decreases with time faster, thanthe CME body velocity. As a result, the difference in the CME body and shock velocities forboth CME groups decreases with time, on average, whereas the distance between these structures
increases. From the calculations in 3D, the shock and the CME body velocities also vary at
11different tempo depending on the time (distance). For five HCMEs, there is good agreement
between the ΔR/Rb (standoff distance) radial distribution obtained within the LASCO C3 fieldfrom calculating the characteristics of CME and the related shock in 3D and the ΔR/Rb obtainedby using the formulas from [Russell and Mulligan, 2002] valid for piston shocks. Here, ΔR is the
distance between the CME body and the shock on the CME axis, Rb is the CME body radius
CME on its axis, R is the distance from Sun center.
TWO TYPES OF RESPONSE OF THE MAGNETOSPHERE TO THE INTERACTION
WITH INTERPLANETARY SHOCKS IN THE GEOMAGNETIC PULSATIONS
Vladimir Parkhomov1, Natalya Borodkova2, Aleksandr Yakhnin3,
Aleksandr Pashinin4, Tsegmed Botulai5
1

Baikal State University Russia, Irkutsk, Russia
Institute of Space Research RAS, Moscow, Russia
3
Polar Geophysical Institute, Apatity, Russia
4
Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
5Institute of Astronomy and Geophysics of the Academy of Science of Mongolia, Ulan-Bator,
Mongolia
2

pekines_41@mail.ru

Results of the study of interaction of 30 events of interplanetary shocks with themagnetosphere for the period 2011–2015 are presented. We found two types of the geomagnetic
response. During 20 sudden storm commencement (SSC) cases occurred under solar wind withvelocity <500 km/s, the shocks were accompanied by geomagnetic pulsations Psc 1-5. In 10 SSC
cases, initiated of the interplanetary shocks propagating at speeds V > 500 km/s, a kind of
precursor was revealed, which is a short duration (3–20 s) burst of geomagnetic pulsations in thefrequency range of 0.2–7 Hz. On the ground, the burst of geomagnetic pulsations was observed
globally, that is, in different local times and different latitudes. On spectrograms obtained at
different locations, the burst often exhibits a similar resonant structure (intermittent increases anddecreases of the spectral power at almost multiple frequencies) with some differences in resonant
frequencies at different stations. The resonant structure of the pulsation spectrum is, possibly,
associated with the interaction of the incident MHD pulse and the ionospheric Alfven resonator.
It is shown that the bursts are observed just before the sharp increase in H component of themagnetic field; this is why it can be considered as the precursor of the sudden storm
commencement. The possible reasons of different geomagnetic response to interplanetary shocks
propagating with different speeds are discussed.
POSSIBLE CAUSES OF SHOCK WAVES GENERATION IN THE SOLAR CORONA
IN THE ABSENCE OF CORONAL MASS EJECTIONS
Victor Eselevich1, Maxim Eselevich1, Ivan Zimovets2
1
2

Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
Institute of Space Research RAS, Moscow, Russia

esel@iszf.irk.ru

We present results of analysis of two solar events SOL2012-10-23T03:13 and SOL201403-06T09:23 associated with solar flares and type II radio bursts but without coronal massejections (CMEs) during shock wave generation. We used the method of constructing the12difference brightness profiles in the UV and EUV channels of AIA/SDO in space and time,
together with an analysis of the type II radio bursts. It is shown that in the SOL2012-1023T03:13 event there was formation and propagation of a compression region, ahead of which acollision shock wave is registered at the distances R<1.3Rs (Rs is the radius of the Sun) from thecenter of the Sun. Based on the data analysis we conclude that a possible cause of thecompression region and the shock wave in this event is a short (pulsed) action of a hightemperature eruptive flux-rope to a surrounding plasma medium. The shock wave can beconsidered initially as a piston-driven shock, but as a freely-propagating blast shock at a laterstage. Initial instability and eruption of the flux-rope may be initiated by emerging magnetic flux,
while its heating may be caused by the magnetic reconnection. We also found the formation andpropagation of a compression region in the SOL2014-03-06T09:23 event, in front of which acollisional shock wave was registered at the distances R<1.3Rs from the center of the Sun.
However, this event has two main differences from the SOL2012-10-23T03:13 event: (1) The
first appearance of the moving compression region was registered in a close vicinity to the flaresite, at the distances DR < 0.01Rs from it, and near a time of a flare peak, around 12 seconds after its
start. The further movement of the compression front was smooth and with decreasing speed; (2) No
plasmoid (jet) ejection was seen in the direction of the compression region and shock wave
movement before and during their formation stage. All this allows us to suggest that a possible causeof the moving compression region and shock wave generation in front of it was the solar flare,
namely a sudden (pulsed) increase of the total pressure associated with the flare energy release.
In this case the shock wave can be considered as a purely freely-propagating blast shock.

ENHANCED PLASMA UPFLOWS DURING THE EMERGENCE OF SMALL ACTIVEREGIONS IN THE SOLAR PHOTOSPHERE
Anna Khlystova1, Shin Toriumi2
1
2

Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
National Astronomical Observatory of Japan

hlystova@iszf.irk.ru

We study the plasma flows in the solar photosphere during the emergence of two small
active regions NOAA 9021 and 10768 by using SOHO/MDI data. The strong plasma upflows at
the initial stage of active region formation are detected. Enhancement of the upflow velocity
begins before the magnetic flux emergence; the maximum negative Doppler velocities reach−1650 and −1320 m/s. The velocity structures have size ~8 Mm in diameter and they exist for
1−2 hours. The observed flows are similar to that of the large active region NOAA 10488. The
structures of enhanced plasma upflows are distinguished from the regular granules andsupergranules in the quiet Sun on the size scale, the velocity values, and the lifetime. Thus, thesimilar parameters of enhanced upflows in the earliest phase of the appearance of small and large
active regions may point to the possibility of the emergence of elementary magnetic fluxes withthe similar initial properties. We used the ideal MHD simulations of the magnetic flux
emergence into the solar atmosphere for investigation of the causes of the enhanced plasma
flows at the initial stage of active region formation. Comparison between the observations andthe simulation shows a striking consistency. We found that there exist two distinct driving forces
for the plasma upflows depending on the evolution stage. Just before the magnetic flux reaches
the photosphere, the enhanced upflows are caused by the gas pressure gradient, while after themagnetic flux appears in the photosphere, the magnetic pressure gradient plays a key role.
13

DETECTING THE SOLAR NEW MAGNETIC FLUX REGIONS ON THE BASE OF
VECTOR MAGNETOGRAMS
Aleksei Golovko, Irina Salakhutdinova
Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
golovko@iszf.irk.ru
isalakh@iszf.irk.ru
golovko@iszf.irk.ru

The advanced method of mapping emerging magnetic flux regions through the multifractal
segmentation of vector photospheric magnetograms is created. It is free from influence of effects
of projection. Maps of the longitudinal component of the field Hz and of the two transversal
components Hx, Hy are processed separately and the computed segmented images are
summarized. As a result, for the first time the detailed picture of distribution of new magnetic
fluxes at the current time, is obtained. The SOT Hinode magnetograms for 2006-2015 were used.
Observations of the flare-productive active regions NOAA 11158, 11263, 11520 and 11589 were
processed. During the periods of rapid development, sites of new magnetic flux are built incellular structures. Hills of a new field in case of their birth have the considerable elongation
which is possibly related to their rope-like geometry. In the centers of flare activity, in thevicinity of polarity inversion lines, exits of new magnetic flux alternate with processes ofmagnetic cancellation.

COMPARISON OF THE MAIN OSCILLATION CHARACTERISTICS
IN THE SOLAR CHROMOSPHERE, SOLAR WIND, AND MAGNETOSPHERE
Andrei Chelpanov, Nikolai Kobanov, Maksim Chelpanov, Sergei Chupin
Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
chelpanov@iszf.irk.ru

The aim of this work is to consider the probable Suns chromosphere source of theoscillations in the solar wind, and to estimate the influence of these oscillations on the pulsations
registered in the magnetosphere. We compare the spectra of the oscillations in the coronal holes
chromosphere with those in the solar wind. The oscillations observed in the chromosphereindicate the probable torsional Alfven wave presence — this mode can propagate long distances
without dissipating in the interplanetary space. Alfven wave signatures are also found in the solar
wind based on the ACE satellite data in the L1 point. We analyze the characteristics of theobtained spectra and estimate the possibility of the wave mode transformation in the process of
propagating through the Sun — solar wind system.

14

INFLUENCE OF CME–CME AND CME–HSS INTERACTIONS ON THE
PARAMETERS OF ICME AT 1AU
Yulia Shugay1, Denis Rodkin2, Farid Goryaev2
1
2

Skobeltsyn Institute of Nuclear Physics, Moscow State University, Moscow, Russia;
P.N. Lebedev Physical Institute, Moscow, Russia

slem@sci.lebedev.ru

Identification of solar sources of the interplanetary coronal mass ejections (ICMEs) for thegrowing phase of cycle 24 (2010–2012) based on the Richardson and Cane ICME list has shownthat in ~30 % cases the observed ICME may be associated with two or more CMEs. Such CMEs
propagating to the Earth can interact in the corona or in the heliosphere. In some other cases,
CMEs can propagate along and interact with high speed streams (HSSs) of solar wind fromcoronal holes. As a result, this interaction can lead to specific changes in the parameters of theassociated ICMEs at 1 AU, such as velocity, magnetic field and ion composition. In the report, weconsider the forming of the ion charge state of the ICME plasma for a typical CME and the scenarios
how interaction of a CME with other solar wind streams (CME, HSS) can influence on the ICME
parameters observed at 1 AU. We demonstrate these effects on a number of cases of cycle 24.
ON GEOEFFECTIVENESS OF CMES DURING SC24
Diana Besliu-Ionescu1, Dana Camelia Talpeanu2, Marilena Mierla1,2,
Georgeta Maris Muntean112Institute of Geodynamics Sabba S Ștefănescu of the Romanian Academy Romania
Royal Observatory of Belgium, Belgium

diana.ionescu@geodin.roCoronal mass ejections (CMEs) are parts of the puzzle that drives space weather.
Numerous methods (theoretical or numerical) are being used to predict whether the CME will begeoeffective or not. By extending a study proposed by Srivastava (2005), we developed a logistic
regression model to predict the probability of geomagnetic storms occurrence Dstmin<–30 nT.
We applied it for events during the ascending phase of solar cycle 24. The results obtained arecompared with similar ones obtained for the ascending phase of solar cycle 23. A summary
describing the observations and methods limitations is also given.
INFLUENCE OF HSS-CME INTERACTIONS ON THE PARAMETERS OF HSS AT 1 AU
Yulia Shugay1, Vladimir Slemzin2, Denis Rodkin2
1
2

Skobeltsyn Institute of Nuclear Physics, Moscow State University, Moscow, Russia
P.N. Lebedev Physical Institute of Russian Academy of Sciences, Moscow, Russia

yushugay@gmail.com

The HSS-CME interactions can lead to the large errors in the forecasts of the arrival time
HSS and the amplitude of the HSS speed, as well as to the absence of the expected CIR. We
investigated the cases of possible HSS-CME interactions in the 24th solar cycle. The changes inthe HSS parameters at 1 AU, such as kinematics, magnetic field and ion composition, were15

examined. In the cases of HSS-CME interactions we determined the degree of discrepancy
between the observed at 1 AU and forecasted parameters. We used WSA-ENLIL model and theempirical solar wind forecast model based on areas and magnetic fields of coronal holes. We
investigated how the detected discrepancy depends on the relative location, magnetic
configuration of the solar sources of HSS and CME.
RELATIONSHIP BETWEEN SOLAR WIND DIFFERENT TYPES AND
LATITUDINAL PROPAGATION OF SUBSTORMS
Irina Despirak1, Andris Lubchich1, Natalya Kleimenova2, Veneta Guineva3
1

Polar Geophysical Institute, Apatity, Russia
Schmidt Institute of the Physics of the Earth RAS, Moscow, Russia
3Space Research and Technology Institute, BAS, Stara Zagora, Bulgaria
2

despirak@gmail.com

Based on the data of the catalog of large-scale solar wind types (ftp://ftp.iki.rssi.ru/omni/),OMNI database by the solar wind and IMAGE magnetometers network we made a comparative
analysis of the conditions of the appearance of substorms at different latitudes. All considered
substorms were divided into different types according to their location in relation to the auroral
oval dynamics. The first type — the substorms which propagate from the auroral geomagnetic
latitudes to the polar ones (called “expanded” substorms, according to an expanded oval
dynamics); the second type — the substorms which are observed only at the geomagnetic
latitudes above ~70 degrees in the absence of simultaneous magnetic disturbances below 70 degrees(called “polar” substorms, according to a contracted oval dynamics). Substorms observed close
to the minimum and maxima the 23th and 24th solar cycles on the meridional chain (Tartu —Ny Ålesund) of IMAGE stations were considered (namely, periods 1995–1996, 2008–2009,
1999–2000 and 2012–2013). We have analyzed the space weather conditions before the onset ofthese two types of substorms. It is shown that in different conditions of space weather,
determined by solar wind large-scale structure, the different types of magnetic substorms occur.
Eхpanded, i.e. moving to north, substorms occur, mainly, during high-speed streams fromcoronal holes, and polar substorms occur during the slow flows and the heliospheric current
sheet, as well as some of the displays of interplanetary coronal mass ejections (ICME).
AN ANALYSIS OF SOLAR ERUPTIVE PROCESSES USING COMBINED EUV
AND RADIO MEASUREMENTS
Vratislav Krupar1,2, Jasmina Magdalenic3, Matthew West3, Elke DHuys3, Lubomir Prech4,
Oksana Kruparova2
1

NASA/GSFC, USA
Institute of Atmospheric Physics CAS, Czech Republic;
3
Royal Observatory of Belgium, Belgium
4Charles University, Czech Republic;2

vk@ufa.cas.cz

The strongest space weather disturbances are linked with Coronal Mass Ejections (CMEs)
and associated shock waves. We performed a multi-wavelength study of selected CME/flare
events using combined extreme ultraviolet (EUV) and radio observations. The unique large fieldof-view EUV observations by Project for Onboard Autonomy 2/Sun Watcher with Active Pixels
16and Image Processing (PROBA2/SWAP) allow us to investigate properties of coronal magnetic
structures over a wide range of time scales, sizes and temperatures. Here, we focus on coronalloops and their magnetic topology, which produce fast electrons responsible for solar radio
bursts. We compare radio source locations observed by Nancay Radioheliograph with
PROBA2/SWAP images to study CME-driven shock wave kinematics.
NEW PROTON EVENT CATALOGS AND STATISTICAL RESULTS
Rositsa Miteva1, Susan W. Samwel2, Marcus V. Costa-Duarte3, Dimitar Danov1,
Katya Georgieva1
1Space Research and Technology Institute of Bulgarian Academy of Sciences, Sofia, Bulgaria
National Research Institute of Astronomy and Geosphysics, Helwan, Cairo, Egypt
3
Institute of Astronomy, Geophysics and Atmospheric Sciences, University of Sao Paulo, Sao
Paulo, Brazil
2

rmiteva@space.bas.bg

In this report we summarize the data analysis, contents and statistical results from three
newly compiled catalogs (1996–2016) of solar energetic protons. Proton data from
Wind/EPACT, SOHO/ERNE and GOES instruments are analyzed. We applied the sameprocedure for the proton intensity enhancement identification and analysis. Namely, we
completed: visual scanning of the data; data smoothing of about 5–10 min; onset time
identification of 3-sigma above background; removal of energetic storm particle contaminations
from the identifications of the proton peaks; onset-to-peak fluence calculation. Solar origin(flares and coronal mass ejections) of the proton events are proposed. Here, we summarize thedifferent trends obtained for the protons and their origin, e.g., with respect to proton energy andintensity, solar origin position and intensity, solar cycle. Finally, we discuss the proton
occurrence probabilities for various ranges of the solar origin parameters.

SOLAR WIND CHARACTERISTICS IN POLAR REGIONS OF THE SUN CORONABY STEREO DATA DURING 2009–2014
Anastasiia Kudryavtseva, Dmitry Prosovetsky
Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
kudryavtseva@mail.iszf.irk.ru

On white-light coronagraphs images inside solar wind flows observed jets — streams ofmatter, driven radially outward the Sun. We analyzed white-light images producing bycoronagraph COR2/STEREO (field-of-view 3.5–16 solar radii) during 2009–2014 years anddetermined jets characteristics in polar regions of solar corona. There were determined sizes andvelocities of jets, their number during researched period. Comparison between all jets
characteristics in south and northern solar hemispheres was done.

17

FLARE ENERGY RELEASE: INTERNAL CONFLICT, CONTRADICTION WITH
HIGH RESOLUTION OBSERVATIONS, AND POSSIBLE SOLUTIONS
Lev Aron Pustilnik
Israel Cosmic Ray and Space Weather Center, Tel Aviv University & Israel Space Agency &Golan Research Institute, Israel
levpust@post.tau.ac.il

All accepted paradigms of solar and stellar flares energy release are based on two whales:
Source of energy is free energy of non-potential force free magnetic field in atmosphere above
active region. Process of ultrafast dissipation of magnetic fields is reconnection in thin turbulent
current sheet (RTTCS). Progress in observational technics in last years provided ultra-highspatial resolution and in physics of turbulent plasma showed that real situation is much more
complicated and standard approach is in contradiction both with observations and with problemof RTTCS stability. We present critical analysis of classic models of pre-flare energy
accumulation and its dissipation during flare energy release from pioneer works Giovanely [1939,
1947] up to topological reconnection. We show that all accepted description of global force-freefields as source of future flare cannot be agreed with discovered in last time fine and ultra-finecurrent-magnetic structure included numerous arcs-threads with diameters up to 100 km withconstant sequence from photosphere to corona. This magnetic skeleton of thin current magnetic
threads with strong interaction between them is main source of reserved magnetic energy in solar
atmosphere. Its dynamics will be controlled by percolation of magnetic stresses through networkof current-magnetic threads with transition to flare state caused by critical value of global current.
We show that thin turbulent current sheet is absolutely unstable configuration both caused by
splitting to numerous linear currents by dissipative modes like to tearing, and as sequence of
suppress of plasma turbulence caused by anomalous heating of turbulent plasma. In result of
these factors primary RTTCS will be disrupted in numerous turbulent and normal plasma
domains like to resistors network. Current propagation through this network will havepercolation character with all accompanied properties of percolated systems: self-organization
with formation power spectrum of distribution of flares and micro-flares, and possibility of phasetransition to flare energy release with huge increasing of energy release.
THE SHOCK WAVE DEVELOPMENT IN A MAJOR SOLAR ERUPTIVE EVENTRESPONSIBLE FOR GLE63
Valentin Kiselev, Victor Grechnev, Arcadiy Uralov, Alexey Kochanov
Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
valentin_kiselev@mail.iszf.irk.ru

The 26 December 2001 solar eruptive event produced a strong particle flux and groundlevel enhancement of cosmic-ray intensity (GLE63). This solar event associated with a moderate
flare and fast coronal mass ejection (CME) was not comprehensively studied because of
insufficient observations. We analyze the shock-wave excitation in this event and its posterior
evolution. We found that two blast-wave-like shocks appeared during the flare impulsive phase.
The first strong wavelike disturbance was impulsively excited by the main eruption close to the
CME onset time. The second one was produced by a jet-like eruption five minutes later. Each18

wave rapidly steepened into a shock due to a steep falloff of the fast-mode speed away from theeruption region. Signatures of type II radio bursts indicate two different shock fronts following
each other. The two shock waves eventually merged around the radial direction into a single
shock. It was traced up to 25 solar radii as a spherical halo ahead of the expanding CME body,and a calculated trajectory of the type II emission matches its total evolution from 80 MHz to
150 kHz. Properties found for the shock wave indicate its intermediate regime between the blast
wave and bow shock in the LASCO field of view. This shock-wave history updates a widely
accepted view on a CME-driven shock: the shock wave actually appears earlier, being able toaccelerate particles to high energies during the flare rise.

ELEMENTARY ACTS OF ENERGY RELEASE IN THE INITIAL STAGE
OF THE 4 AUGUST 2011 FLARE
Nataliia Meshalkina1, Alexander Altyntsev1, Hana Meszarosova2, Marian Karlicky2,
Sergey Lesovoi1
12Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
Astronomical Institute of the Academy of Sciences of the Czech Republic, Czech Republic

nata@iszf.irk.ru

Observations with the high temporal resolution in microwave and X-ray ranges allowed us
to find groups of sub-second pulses (SSP) in the interval lasting 5 min (uniquely long) before theimpulsive phase of the 4 August 2011 (M9.3) flare. The sources of all SSP are located near the
top of a flare loop, however spectral characteristics of pulses differed in the individual groups. In
the first two groups pulses were observed synchronously in the wide range of microwave and
HXR radiation. The third group was narrow-band. In the second group which was observed
during sub-burst intensity of broadband impulses was large enough to measure a spectrum.
Temporal profiles of sub-burst were modulated by broadband multiperiodic pulsations in the
microwave radiation (2–17 GHz, NORP data) and X-ray radiation (HXR) (4–100 keV, FERMI data)with the periods of several seconds. The spectral behavior of the microwave and X-ray emissions
during quasi-periodic pulsations are analyzed. Probable mechanisms of SSPs and relationship withplasma parameters obtained from microwave and HXR spectra during SSPs are discussed.
SXR SOLAR FLARES DURING MINIMUM OF SOLAR ACTIVITY
Magdalena Gryciuk1,2, Marek Siarkowski1, Janusz Sylwester1, Szymon Gburek1,
Piotr Podgórski1
1
2

Space Research Centre Polish Academy of Sciences, Solar Physics Division, Poland
Astronomical Institute, University of Wroclaw, Poland

mg@cbk.pan.wroc.pl

Sphinx was the Polish X-ray spectrophotometer designed to measure X-ray emission fromthe Sun in the energy range between 1.2 and 15 keV. The instrument was placed onboard
Russian CORONAS-Photon satellite which was launched on January 30, 2009. SphinX mission
operated from February to November 2009 and provided large database of flare observations.
These data are used for the analysis of flares’ light curves as seen in soft X-ray. We will present
analysis results for selected events.
19

STEADY ANISOTROPIC OUTFLOWS: THE 16-MOMENTUM
MHD APPROXIMATION
Mahir Sh. Pirguliyev, Namig Sardar Dzhalilov
N. Tusi Shamakhy Astrophysical Observatory, Azerbaijan National Academy of Sciences, Baku,
Azerbaijan
mahir.p@shao.az

Observations and measurements of space plasma in the regions, such as the ionosphere, theEarths magnetosphere, and the solar wind show the presence of the temperature anisotropy of theplasma relative to the direction of the magnetic field. This property has a collisionless plasma ina magnetic field. Such conditions are realized in the plasma of the upper solar corona, where
there are enough sources to create and maintain the plasma temperature anisotropy. For thatenvironments, the particle distribution function (especially ions) is non-Maxwellian and at small
collisions, isotropic MHD equations are not applicable. For the MHD description of such aplasma is widely used equations of Chew-Goldberger-Low (CGL) model. However, theseequations do not take into account the heat fluxes that occur naturally along the magnetic field ina collisionless plasma and contain artificially introduced two adiabatic invariants. Consequently,
these equations cannot describe such important compressible instability as a mirror and a second
firehose instabilities. To study the effects associated with heat flux along the magnetic field, it ispossible to use the most common MHD transport equation for the anisotropic plasma, which was
obtained by many authors as equations for the 16-momentum of the distribution function ofparticles. In this paper, we used the full set of the 16-momentum MHD equations that take into
account the heat fluxes along the magnetic field in an anisotropic plasma of the solar wind. 16momentum MHD equations have been used by many authors in theoretical studies, especially forthe modeling of the solar wind and studying the wave instabilities of an anisotropic plasma.
Parker developed the supersonic model for the expansion of the solar wind, but this model
describes the solar wind only in general. In this paper, we summarized Parkers problem, taking
into account the anisotropy of the solar wind plasma. We found particular analytical solutions of
the obtained equations in both 16-momentum MHD and CGL-MHD models. We obtain a quasilinear Parker-type differential equation for the outflow speed whose solution topology isnumerically found with an evolution law of the temperatures such that T= T0(r/r0) – β and T== T0(r/r0) – β . We describe possible critical points both physical and unphysical in these models.
Different cases are discussed by the set of constant parameters β and β and of the anisotropy atthe base r0 of the corona. In particular, we discuss the isothermal case.

20

KELVIN—HELMHOLTZ INSTABILITY BETWEEN SOLAR WINDS COMPONENTS
IN 16-MOMENTUM MHD FORMALIS
Rajab Ismayilli1, Namiq Dzhalilov1, Bidzina Shergelashvili2,3, Stefaan Poedts4,
Mahir Pirguliyev1
1

Shamakhy Astrophysical Observatory of the ANAS, Baku AZ-1000, Azerbaijan;
Abastumani Astrophysical Observatory at Ilia State University, Kakutsa Cholokashvili Ave 3/5,
Tbilisi, Georgia
3
Combinatorial Optimization and Decision Support, KU Leuven campus Kortrijk, Sabbelaan 53,
8500 Kortrijk, Belgium
4Space Research Centre for Mathematical Plasma Astrophysics, Department of Mathematics, KU
Leuven, Celestijnenlaan 200B, 3001, Leuven, Belgium
2

rajab.i@shao.az

We analyze wave instabilities in a magnetized, anisotropic, and collisionless plasma in thefluid approximation using the 16-momentum MHD formalism. In this work, we present simple
configuration of tangential discontinuity with a possibility to choose some special cases when to
parameters of plasmas such as the pressure, density, initial heat fluxes, plasma-beta, andanisotropy are given physical mean values. We discuss the cases when interfaces between solar
winds components are Kelvin—Helmholtz unstable, by including dimensionless parameter$h$ as the ratio of flow speeds, which values provide enough condition for velocity shear acrossthe interfaces. As a first step, we eliminate the heat flux, and select the same physical parameters
in both flows, and solve the dispersion equation. The task parameters for supersonic flows werechosen so that to filter out classic firehose and mirror (during quasi-transverse propagation)
plasma instabilities. It turned out that KHI increment, unlike the usual hydrodynamic case, hasmaximum, and the instability has two thresholds in the anisotropic case. In other words, KHI
occurs within h1<h<h2, where h=V01/V02 characterizes the ratio between the flow velocities.
MULTI-INSTRUMENT ANALYSIS OF SOLAR ERUPTIVE EVENTS OBSERVED BY
THE SIBERIAN RADIOHELIOGRAPH AND COMPARISON WITH TRADITIONAL
HYPOTHESES: DEVELOPMENT OF A SHOCK WAVE AND CME
Victor Grechnev, Sergey Lesovoi, Alexander Altyntsev, Alexey Kochanov,Arkadiy Uralov, Alexey Gubin, Dmitry Zhdanov, Eugene Ivanov, Larisa Kashapova
Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
grechnev@iszf.irk.ru

The first 48-antenna stage of the Siberian Radioheliograph (SRH) constructed on the baseof the SSRT started observing the Sun in 2016 initially in a single-frequency mode and sinceAugust at five frequencies in the 4-8 GHz range. We firstly present an unprecedented series ofnegative bursts observed within one day on 9 August, which were caused by screening acompact microwave source by repetitive surges visible in extreme ultraviolet. Then we focus onan eruptive C2.2 flare on 16 March 2016 around 06:40, one of the first flares observed by SRH.
We analyze this event using imaging and non-imaging radio, extreme-ultraviolet, hard X-ray,and white-light data, endeavoring to reveal its scenario and compare the observational resultswith expectations from traditional hypotheses and our recent conclusions. An eruptive
prominence actively expanded, twisted, writhed, and brightened. This behavior rules out apassive role of the prominence, indicating development of its violent instability. A flux rope
appears to have been formed from the prominence and developed into a large CME. The
21

prominence eruption caused a weak impulsive flare with a conspicuous hard X-ray burst at > 70 keV
and a weak microwave burst of 15 sfu. The burst clearly lagged behind the prominence lift-off,as we observed in different events. The impulsive prominence eruption excited a shock wave,
which appeared during the impulsive burst and was manifested in an “EUV wave” and Type II
radio burst. The observations indicate a multi-component structure of non-thermal microwave
and hard X-ray sources and demonstrate that an impulsive flare is not necessarily confined.
STUDY OF MAGNETIC STRUCTURE AND TRIGGER MECHANISM FOR SOLAR
FLARE
Johan Muhamad, Kanya Kusano, Satoshi Inoue, Daikou Shiota
Institute for Space-Earth Environmental Research, Nagoya University, Japanjohanm@isee.nagoya-u.ac.jp

As the largest eruption in the solar system, solar flare can release large amount of energythat may disrupt satellite and spacecraft operations and may impact social aspects in the modern
life. It is essential to enhance the capacity of flare prediction in order to get the better prediction
result. Therefore, we studied magnetic structure of active regions, which produced large solar
flares, with regard to understand the flare trigger mechanism. Nonlinear Force Free Field(NLFFF) extrapolation method was used to model the coronal magnetic field of the active
regions NOAA 10930 and 11158 based on the photospheric magnetogram data from Hinode andSDO satellites. We found that the magnetic fields of the flare-productive active regions werehighly sheared near the Polarity Inversion Line (PIL) before the large flares happened. We usedthe coronal model as an initial condition for performing MHD simulation to study the trigger
mechanism. By imposing bi-pole structure with various orientations, we found that there are two
type of structure that can effective to trigger the flare. They are opposite polarity (OP) andreverse shear (RS) type structure which emerge onto the highly sheared magnetic fields. This
result is consistent with the previous study done by Kusano et al. (2002) who studied the trigger
mechanism for the Linear Force Free Field magnetic structure. Moreover, by comparing thesynthetic flare ribbons from the simulation with the observation, we could determine which
possible type of trigger structure responsible for triggering the flare. We also calculated a newparameter that can show the averaged twist of magnetic field lines normalized by the totalmagnetic flux within AR from the NLFFF model. We found that this parameter is varied during
the evolution of the active region and dramatically decreased after the onset of the flare. Finally,
we discuss that this parameter may be informative for flare prediction.
THE ORIGIN OF SOLAR FLARES AND CMES: ADVANCES AND CHALLENGES
Larisa Kashapova
Institute of Solar Terrestrial Physics SB RAS, Irkutsk, Russia
lkk@iszf.irk.ru

The main drivers connecting the Sun with the interplanetary space and the terrestrial
atmosphere during the extremal transient events are the solar flares and the coronal massejections (CMEs). Undoubtedly, understanding of the reasons and scenarios of these phenomena
onset is the key initial condition for analysis and interpretation of various geoeffective
disturbances. Nowadays we know a lot about the reasons and mechanisms driving to origin both
22

the flare and CME but some details of puzzle are still unknown. In current contribution we will
present the observational facts and theoretical models explaining both qualitatively andquantitatively these phenomena. Our attention will be focused on analysis of what we have
known and what we doubt or need to investigate.
ANALYSIS OF THE DIFFERENTIAL EMISSION MEASURE EVOLUTION FOR
SOLAR FLARES OBSERVED BY RESIKAnna Kepa1, Magdalena Gryciuk1,2, Barbara Sylwester1, Janusz Sylwester,Marek Siarkowski1
1

Space Research Centre Polish Academy of Sciences Solar Physics Division 51-622 Wrocław,

Poland2

Astronomical Institute, University of Wroclaw, Poland

ak@cbk.pan.wroc.pl

The X-ray spectrometer RESIK observed the spectra in four wavelength bands from 3.3 to
6.1 Å. This spectral range contains many emission lines of H- and He-like ions for Si, S, Ar and
K. These lines are formed in the plasma of coronal temperatures (T > 3 MK). The analysis ofobserved lines’ intensities allows to study the differential emission measure distributions (DEM)
in the temperature range between 3 and 30 MK. In this contribution, we analyze the timechanges of the DEM distributions for successive flares observed with the RESIK instrument. The
model of the elementary flare profile (EFP) has been used in order to separate the individualflares based on their observed light curves.
DIAGNOSTIC OF THE TEMPERATURE DISTRIBUTION IN CORONALSTRUCTURES ABOVE SUNSPOTS, USING 3-MIN OSCILLATIONSAnastasiya Deres
Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
deres@mail.iszf.irk.ru

In this research we investigate the possibility of applying slow MHD waves for the
diagnostic of the transverse temperature distribution in coronal structures above sunspots. Since
the coronal EUV emission is optically thin, any EUV imaging instrument (like SDO/AIA)
emission along the line of sight from the entire of an active region. Therefore, the interpretationof EUV observations is a challenging task. To determine the influence of the transverse
temperature distributions in coronal structures to the observation of the slow MHD wave
propagation, we apply the forward modeling approach. We apply the FoMo code, which uses thevolume distribution of plasma parameters (temperature, density and plasma velocity) as an input.
We performed three numerical MHD simulations of the slow wave propagation in coronal
structures with uniform, hot, and cold interiors, and made synthetic EUV images for different
wavelengths. The images were investigated in detail and compared with real SDO/AIA
observations of slow MHD waves in coronal structures above sunspots. Specific features thatallow us to distinguish between different temperature distributions were revealed and discussed.

23

LINK BETWEEN SLOW-MODE MHD WAVES AND QPPS IN SOLAR FLARES:
MODE TRANSMISSION MECHANISM
Andrey Afanasyev, Arkadiy Uralov
Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
afa@iszf.irk.ru

Recent observations of magnetohydrodynamic oscillations and waves in solar active
regions revealed their close link to quasi-periodic pulsations in flaring light curves. The nature ofthat link has not yet been understood in detail. In our analytical modelling we investigate
propagation of slow magnetoacoustic waves in a solar active region, taking into account wave
refraction and transmission of the slow magnetoacoustic mode into the fast one. The wave
propagation is analysed in the geometrical acoustics approximation. Special attention is paid tothe penetration of waves in the vicinity of a magnetic null point. The modelling has shown thatthe interaction of slow magnetoacoustic waves with the magnetic reconnection site is possible
due to the mode transmission at the equipartition level where the sound speed is equal to the
Alfvén speed. The efficiency of the transmission is also calculated.

FLUENCE SPECTRA OF SMALL SEP EVENTS WITH METRIC TYPE II RADIO
BURSTS
Pertti Makela1, Nat Gopalswamy2, Sachiko Akiyama1, Seiji Yashiro1
1
2

The Catholic University of America, Washington, DC 20064, USA
NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA

pertti.makela@nasa.gov

Gopalswamy et al. (2016, Astrophysical Journal, 833, 216) showed that the spectral index
of the 10–100 MeV proton fluence spectra organizes the major solar energetic particle (SEP)
events. Ground level enhancement (GLE) events and SEP events associated with filament
eruptions outside active regions (FE SEP events) have respectively hard (gamma ~2.68) and soft
(gamma ~4.89) fluence spectra. Between these two distinct groups fall the regular SEP events(gamma ~3.83). Here we report on a study of proton fluence spectra of small SEP events, i.e.
events with the GOES 10 MeV peak flux below 10 pfu, that have an associated metric type II
radio burst during solar cycle 24. We utilize the low-background measurements by the Energetic
and Relativistic Nuclei and Electron (ERNE) instrument on the Solar and Heliospheric
Observatory (SOHO). Preliminary results show that the distribution and the average value ofspectral index of small SEP events resemble those of the regular SEP events.

24THE ORIGIN AND PROPAGATION OF SOLAR ENERGETIC PARTICLESAND THEIR IMPACT ON EARTH
Silvia Dalla
University of Central Lancashire, Preston, United Kingdom
sdalla@uclan.ac.uk

Solar eruptive events generate Solar Energetic Particles (SEPs) which, by propagating
through the interplanetary medium, may reach near-Earth space. SEPs are an importantcomponent of Space Weather and produce a variety of effects, including posing a significant
radiation risk to humans in space and satellite hardware. This talk will review our understandingof the origin and propagation of SEPs, based on a large body of data gathered by spacecraft andground-based detectors and on theoretical models. It will describe processes by which particle
acceleration takes place near the Sun and within the interplanetary medium. Particle transport
through the interplanetary medium will be discussed, including the role of the large scale
magnetic field configuration and of the superimposed turbulence, which produces scattering andfield line meandering. Impacts of SEPs on the near-Earth environment will be reviewed.
THE MULTIWAVE SIBERIAN RADIOHELIOGRAPH: IMAGING SOFTWAREAND CALIBRATION
Anastasiia Fedotova, Alexey Kochanov, Sergey Lesovoi, Alexander Altyntsev,
Victor Grechnev
The Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
fedotovanastya@mail.iszf.irk.ru

In the year 2016 multiwave observation of the Sun with the Siberian Radioheliograph(SRH-48) in the frequency range 4–8 GHz started. It gives new possibilities for investigation ofplasma and magnetic fields in solar corona, accelerated particles, coronal mass ejection, eruption
phenomena and other manifestations of solar activity. The methods of processing and calibration of
the raw data are presented. The examples of synthesized radio maps of the Sun at several frequencies
were compared with solar images obtained at other instruments such as NoRH and AIA/SDO.
PC INDEX AS A PROXY OF THE SOLAR WIND ENERGY THAT ENTEREDINTO THE MAGNETOSPHERE IN CASE OF MAGNETIC STORMS
Oleg Troshichev, Dmitry Sormakov
Arctic and Antarctic Research Institute St. Petersburg, Russia
olegtro@aari.ru

Magnetic storms with intensity Dst < –30 nT observed in epoch of 1998–2015 (N=431)
have been analyzed. The 1-min SymH index smoothed with use of the running window of 30 min
width was examined as a storm characteristic. The 30-min smoothed PC index was derived in asimilar manner. The storms were classified into 3 categories according to features of the PC
index behavior in course of storm, as follows: (1) storms with the well-defined regular PC index
25increase above the threshold level ~1.5 mV/m, (2) storms with the periodically oscillating PC
index, and (3) storms with imposition of the PC index oscillations on the PC index enlargement(composition of two first categories). The analyzed magnetic storms were compared withcatalogues of the (Interplanetary) coronal mass ejections (ICMEs/CMEs) and stream (corotating)interaction regions (SIR/CIRs), which are known as the solar wind drivers of magnetic storms. It
is shown that storms of the 1st category are commonly related to CME/ICME events, the stormsof the 2nd category are related exclusively to SIR (CIR) events, whereas the composite storms
are associated with both solar wind drivers. Relationships between the 30-min smoothed PC and
SymH indices were examined for all categories of storms at interval ΔT=Tmax±48 hours, where
Tmax is a moment of maximum storm intensity (i.e. moment of maximal depression ofgeomagnetic field). Results of the statistical analysis demonstrate that depression of geomagnetic
field (Dst variation) starts to develop as soon as PC index steadily excess the threshold level of~1.5 mV/m, like to case of magnetic substorms. SymH index in course of magnetic storm
generally follows the time evolution of the smoothed PC index with typical delay time of ~(1±0.5) hour. The storm intensity (Dstmin) is linearly related to maximal value of the hourly mean
PCMAX value observed about 1 hour before the moment of maximal depression. The conclusion
is made that the PC index can be successfully used for now casting the magnetic storm
development.
DIAGNOSTICS OF SOLAR CORONAL PLASMAS WITH RAPIDLY-PROPAGATINGQUASI-PERIODIC WAVE TRAINS
Valery Nakariakov
University of Warwick, United Kingdom
V.Nakariakov@warwick.ac.uk

Rapidly-propagating quasi-periodic wave trains of the EUV emission intensity variations
recently discovered in coronal active regions, and associated quasi-periodic radio bursts, provide
us with a tool for the diagnostics of the magnetic connectivity in the solar atmosphere. In
particular, a wave train observed during the impulsive phase of an M1.9 flare on 7 May 2012
with SDO/AIA in 171 and 193 Å passbands, had a period of about 140 s, and apparent instantphase speed of 660–1400 km/s. Simultaneously, quasi-periodic variations of the time derivativeof the GOES soft X-ray flux were found to have a 70-s period. Similar periodicities weredetected in the metric/decimetric (245/610 MHz) radio bursts at several ground-based stations of
RSTN. Wave trains are shown to occur as a response of coronal magnetoacoustic waveguides oranti-waveguides to an impulsive energy deposition, e.g. bursty magnetic reconnection. The
observed properties of the wave trains, such as wavelet spectra, are determined by the dispersive
properties of the waveguides, prescribed by the plasma and magnetic field non-uniformities.
Full-MHD numerical simulations of the evolution of broadband fast magnetoacoustic pulses
show good agreement with the observed properties of fast wave trains. Thus, the frequency andamplitude modulations in the fast wave trains, determined, in particular, with the use of thecharacteristic tadpole wavelet signatures, and their evolution with time and along the wave pathgive us information about the plasma structuring. The direction of the wave train propagation,
together with the estimation of the local plasma density by the frequency in the radio band,
reveals the communication channel. However it is important to distinguish between the guided
and leaky parts of the fast magnetoacoustic perturbation. In addition, it is found out that theobservational manifestation of fast wave trains is strongly affected by the line-of-sightintegration effect that has to be taken into account in the interpretation of observations.
26

MHD-SEISMOLOGY OF THE CORONAL MAGNETIC FIELD BY DECAY-LESSKINK OSCILLATIONSSergey Anfinogentov1, Valery Nakariakov2
1
2

Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
University of Warwick, United Kingdom

anfinogentov@iszf.irk.ru

The magnetic field controls almost all processes in the corona, including the accumulationof energy and its release during flares and coronal mass ejections. Hence its knowledge is the
key ingredient of solar activity and space weather forecasting. However, the practical applicationof the existing methods for the estimation of the magnetic field in the corona(radiomagnetography, extrapolation of the photospheric field and MHD seismology) is limited
by some complex difficulties. As a result, there are still no regular and reliable measurements ofthe coronal magnetic field. MHD seismology provides a possibility for the measurement of thecoronal magnetic field by using MHD waves in the coronal plasma as natural probes. Standing
kink oscillations of coronal loops are the most promising tools for measuring the coronalmagnetic field, because the magnetic field can be easily calculated from the observed parameterssuch as the oscillation period, the length of the loop, density contrast, and plasma density inside
the loop. Up to the present time, observations of decaying kink oscillations of coronal loops havebeen relatively rare. These events are mainly associated with solar flares and CMEs, and hence
occur occasionally. Therefore, they are not suitable for the routine seismological diagnostics ofall solar active regions. In this work, we focus on the recently discovered decay-less regime ofkink oscillations that is a ubiquitous phenomenon and can be observed in almost any active
region. Hence, it can be used as a seismological tool for routine diagnostic of the coronalmagnetic field. Decay-less kink oscillations are difficult to detect and to analyse due to their low
amplitude (~0.2 Mm). Hence, we apply the motion magnification method to the observational data.
This technique acts as a microscope, artificially magnifying low amplitude motions in an image
series. It makes low amplitude oscillations easily visible in animations and time-distance plots,
allowing for reliable measurements of their periods. Plasma density inside the loop and the density
contrast are then estimated using the differential emission measure analysis. In combination with theknowledge of the loop length estimated in the assumption of a semi-circular shape of the loop, theseparameters allow us to calculate the magnetic field. We applied this approach to measure themagnetic field in the corona of several active regions, showing the practical possibility of regular of
the coronal magnetic field diagnostics by analysing decay-less kink oscillations.
SYMPATHETIC FLARE ERUPTION USING HIGH RESOLUTION OBSERVATIONS
Aabha Monga
Aryabhatta Research Institute of Observational Sciences (ARIES), Nainital, India
aabhamonga89@gmail.com

We report sympathetic flare events observed in region NOAA AR 12268. Our observation
includes the multi-wavelength study using space instrument like SDO as well as ground based
H-alpha data of ARIES, Nainital. We have not found any signature of filament associated withthese events. Precursor phase study has been done for the triggering and energy generation
mechanism of the flare. Very poor CMEs has been observed along with respective events withthe speed of 222 and 321 km/s. Our investigation reveals the magnetic field emergence and shear
in the active region during its span.
27

MINGANTU SPECTRAL RADIOHELIOGRAPH FOR SOLAR TERRESTRIAL
CONNECTIONSYihua Yan, Wei Wang, Fei Liu, Zhijun Chen, Lihong Geng, Linjie Chen
National Astronomical Observatories, Chinese Academy of Sciences, China
yyh@nao.cas.cn

To address fundamental processes in the solar eruptive phenomena and their geo-effects, it
is important to have imaging-spectroscopy over wide frequency range from the Sun to theinterplanetary space. The Chinese Spectral Radioheliograph (CSRH) is a solar-dedicatedinterferometric array with a frequency range from 400 MHz to 15 GHz. There are two arrays of
40 4.5-m antennas covering 400 MHz – 2 GHz, and 60 2-m antennas covering 2–15 GHz
including antennas, receivers, and correlators which have already been established recently in
Mingantu Town, Inner Mongolia of China. CSRH is renamed as Mingantu Spectral
Radioheliograph (MUSER) after its completion. We introduce the perspectives of MUSER withhigh spatial resolution, high time resolution, and high frequency resolution for solar flare studies.
Some initial results will be presented. The plan to extend MUSER to ~40–400 MHz frequency
regime will also be described so that geo-effective solar radio bursts can be better addressed.

2.5D SIMULATION OF MAGNETOHYDRODYNAMIC WAVE PROPAGATION AND
ITS INTERACTION WITH A CORONAL HOLE
Isabell Piantschitsch1, Bojan Vrsnak2, Birgit Lemmerer1, Arnold Hanslmeier1,
Tomislav Zic2
1
2

IGAM, University of Graz, Institute of Physics, Austria
Hvar Observatory, Zagreb, Croatia;

We developed a new numerical code that is able to perform 2.5D simulations of amagnetohydrodynamic (MHD) wave propagation in the corona and its interaction with a low
density region like a coronal hole (CH). We show that the impact of the wave to the CH leads toeffects like e.g. reflection and transmission of the incoming wave or stationary features at the CH
boundary. We present a comprehensive analysis of the morphology and kinematics of thesecondary waves and their primary counterparts, i.e. we describe in detail the temporal evolutionof density, magnetic field, plasma flow velocity, phase speed and position of the amplitude.
Effects like reflection, refraction and transmission of the wave strongly support the theory thatlarge scale disturbances in the corona are fast MHD waves and build the major distinction to thecompeting pseudo wave theory. Our simulation code is based on the so called Total Variation
Diminishing Lax-Friedrichs (TVDLF) scheme, which is a fully explicit method and is proved tobehave well near discontinuities.

28

ULF BURSTS ACCOMPANYING SOLAR WIND SUDDEN IMPULSES
Battuulai Tsegmed1, Alexander Potapov2
1
2

Institute of Astronomy and Geophysics, Mongolian Academy of Science, Mongolia
Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia

tseg@iag.ac.mn

In this paper we analyzed the ULF bursts observed on April 23, 2002 immediately after asudden magnetic impulse, caused by impact of the solar wind pressure jump on the Earth’s
magnetosphere. Polar measurements of plasma parameters and the magnetic and electric fields
and simultaneous induction magnetometer data from the Sayan and Borok mid-latitude
observatories were used. Polar satellite and the Sayan observatory were located at the moment ofregistering the burst near the midday meridian. Comparison of temporal variation and dynamic
spectra of oscillations on the Earth and in space with variations in particle fluxes and theiranisotropy made it possible to assume that as a result of the action of a sudden impulse, an
excitation of a burst of ion cyclotron waves occurred. A packet of these waves ran along themagnetic field line to the conjugate point in the ionosphere, and then propagated in theionospheric waveguide. These results are compared with another June 28, 1999 event, also
associated with a sudden impulse. In this case, the pattern of the dynamic spectrum of the burst is
characteristic not of ion cyclotron, but fast magnetosonic waves. Possible mechanisms for theexcitation of bursts of either type are discussed.

MULTI-WAVELENGTH IMAGING OBSERVATIONS OF SOLAR BURSTSFROM A PECULIAR RING FLARING REGION ON 2014 DECEMBER 17
Xingyao Chen1, Yihua Yan2, Jing Huang2, Baolin Tan2, Wei W.2
1

National Astronomical Observatories of Chinese Academy of Sciences;
Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of
Sciences, Beijing 100012, China
2

yyh@nao.cas.cn

The multi-wavelength imaging observations of the solar eruptions such as solar flares
provide a method to diagnose the thermal and non-thermal radiation from the sun to theinterplanetary space. Especially, the radio observations allow us to better understand theevolution of the flare eruption and its associated hypothesized electron acceleration sites, from
eruption initiation to propagation into the corona. In this work, we present multi-wavelength
imaging observations to analyse a M8.7 flare in a peculiar ring active region on 2014 December
17, such as the complicated loop systems and the associated eruptions in this particular ring
active region in EUV wavelength (AIA/SDO), the imaging of microwave (NORH), X-ray(RHESSI) and radio source(MUSER), the fine structure of the radio dynamic spectrum and therelated CME, and also show the discussions of the possible physical mechanisms and theconnectivity of the multiple loop systems in/around the ring flaring region.

29

SOLAR K-CORONA POLARIMETRY OBSERVATIONS WITH METIS SOLAR
ORBITERMarta CastiOATO INAF, Italy
casti@oato.inaf.it

The study of the origin and the evolution of the dynamical phenomena taking place in thesolar corona is the starting point for understanding their effects on the space weather of the Solarsystem. The solar wind and the coronal mass ejections (CMEs) propagate from the inner
atmosphere of the Sun throughout the edges of the outer solar system, affecting the Earthenvironment and varying the conditions of the heliosphere. In order to characterize and model
the coronal phenomena it is necessary to investigate the most relevant physical parameters of thecorona, such as electron and ion densities, temperatures, and outflow velocities, as well as themagnetic field. The coronal electron density can be measured by observing the polarized broadband visible-light emission of the K-corona. The polarized brightness (pB) of the K-corona
provides a measurement of the electron density integrated along the line of sight. The radial
speed of the neutral hydrogen in the solar wind could be derived by observing the HI Lymanαline-emission. The Metis coronagraph of the ESA/NASA mission Solar Orbiter, will observe theSun closer than ever (up to 0.28 AU).
From this vantage point, Metis will observe for the first time simultaneously the full solar
corona in the linearly polarized, broad-band visible light (580–640 nm) and in the narrow-band
ultraviolet HI Lyman-α (121.6 nm). The scientific objective of the VL channel is themeasurement of the coronal electron density. This quantity is the cornerstone measurements forderiving all the other physical parameters of the corona such as the solar wind speed from UV
observations of the HI Lyman-α. This presentation describes the Metis polarimeter and the
expected performances in measuring the K-corona pB to derive the coronal electron density. The
observation of the K-corona’s pB has the advantage over that of its sole brightness of reducing
the coronal background and foreground along the line-of-sight, improving in this way thecontrast of the coronal images. This presentation will illustrate this advantageand theimplications for future space-weather instrumentation.

CONNECTION BETWEEN MAGNETIC FIELD TOPOLOGYAND CHEMICAL ANOMALIES IN STELLAR CORONAS
Valerii Pipin, Vladimir Tomozov
Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
pip@iszf.irk.ru

We show that abundance of the chemical elements with the low first ionization potential(FIP) in corona of the late-type stars can be connected with the topological characteristics of thelarge-scale magnetic field. In particular, the solar-type stars shows the increase abundance of the
low FIP elements relative to elements with the high FIP with the field). The branch of the fully
convective stars demonstrates the different type of the large-scale magnetic activity. Those stars
reveal the opposite phenomenon. Namely, they show the decreased abundance of the low FIP
elements relative to the elements with the high FIP. Also, in the fully convective stars this effectseems to be saturated and it is independent on magnitude of the large-scale magnetic field.
30

COMPARISON OF CORONAL AND PHOTOSPHERIC ACTIVITY
OF A VERY QUIET SUN
Szymon Gburek1, Magdalena Gryciuk2
1
2

Space Research Centre, Polish Academy of Sciences, Warszawa, Poland
Astronomical Institute, University of Wroclaw, Wroclaw, Poland

sg@cbk.pan.wroc.pl

We compare coronal and photospheric observations during very low solar activity in the
period from February until November 2009. For investigations of the activity in the photosphere,
we use Debrecen Photoheliographic Data. For studies of coronal activity, we review light curves
from The Solar Photometer in X-Rays (SphinX) and Synoptic Composite Image Archive of X-Ray
Telescope (XRT) on Hinode spacecraft. Results of data analysis show, once again, theimportance of short wavelength solar observations in space weather nowcasting and forecasting.

THE LAMBDA EFFECT AND DOUBLE-CELL MERIDIONAL CIRCULATIONSTRUCTURE ON THE SUN
Valery Pipin
Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
pip@iszf.irk.ru

Recent advances in the mean-field models of the solar differential rotation show apossibility for the double-cell meridional circulation pattern which could operates in eachhemisphere of the solar convection zone. This finding is also suggested by the direct numericalsimulations and by some results from helioseismology. In particular, Bekki & Yokoyama (2017)
showed that the double-cell circulation pattern can results from inversion of sign of the nondiffusive part of the radial angular momentum transport in the lower part of the solar convection
zone. Here, we argue that this inversion of sign of the Λ effect results from the radial gradientsof the Coriolis force acting on the convective flows. Employing the standard solar interior model
as input, we construct a model of solar differential rotation which shows the double-cell
meridional circulation pattern. Developing this model further, we show results for a dynamically
self-consistent nonlinear dynamo model which take into account the magnetic feedback effect on
the differential and the meridional circulation.

31Session 2: LONG-TERM VARIATION OF THE SUN, GEOMAGNETIC
ACTIVITY, AND CLIMATE_____________________________________________________________SUNSPOT NUMBER SERIES REVISITED: WHERE ARE WE?
Ilya Usoskin
University of Oulu, Finland

Until recently, the sunspot number (SN) series known as Wolf (WSN) or International(ISN) one, was the gold standard for generations of scientists to represent solar variability. Later,a group sunspot number (GSN) series was produced by Hoyt and Schatten (1998). However, as
became clear lately, both earlier SN series need revision. Revisions were made in different
directions leading to diverse SN reconstructions which differ essentially between each other. At
present, seven different SN/GSN series circulate around, with a lack of a consensus one. Various
SN series differ in the following issues: Datasets: while WSN/ISN series are not fully
reproducible, since the raw information is not available, GSN series are based on a raw data
database, which has been recently updated; Methodology: Two different methods are used tocompile a composite SN series: daisy-chain linkage and direct active-day fraction method;
Calibration: While most of the old series were based on the linear k-factor (ordinary least square
regression forced through the origin) calibration of different observers, modern conversion
matrix method has been developed; Verification: Many series do not provide a realistic estimateof uncertainties, some other do. Accordingly, the output of various series may differ significantly
between each other. The present level of knowledge of the long-term sunspot variability is quite
uncertain, and collective efforts are needed to reach a community consensus. The current statusof the SN reconstructions for the last century is presented here with an outline of advantages anddisadvantages of different approaches.
CURRENT STATUS OF SCOSTEP/VARSITI — VARIABILITY OF THE SUN
AND ITS TERRESTRIAL IMPACT (2014–2018)
Kazuo Shiokawa1, Katya Georgieva2
1
2

Institute for Space-Earth Environmental Research, Nagoya University, Japan
Space Research and Technologies Institute, Bulgarian Academy of Science, Bulgaria

shiokawa@nagoya-u.jp

The Scientific Committee On Solar-TErrestrial Physics (SCOSTEP) operates the uniquescientific program “Variability of the Sun and Its Terrestrial Impact” (VarSITI) in 2014–2018 to
focus on the recent and expected future solar activity and its consequences for Earth, for various
time scales from the order of thousands years to milliseconds, and for various locations and theirconnections from the solar interior to the Earth’s atmosphere. Four scientific projects are carriedout under the VarSITI program: (1) Solar Evolution and Extrema (SEE), (2) International Studyof Earth-Affecting Solar Transients (ISEST/MiniMax24), (3) Specification and Prediction of the
Coupled Inner-Magnetospheric Environment (SPeCIMEN), and (4) Role Of the Sun and the
Middle atmosphere/thermosphere/ionosphere In Climate (ROSMIC). In order to elucidate
various Sun-Earth connections, VarSITI has encouraged close communications between solar
scientists (solar interior, atmosphere, and heliosphere) and geospace scientists (magnetosphere,
ionosphere, and atmosphere). We have carried out observation/data analysis campaigns for32particular intervals, such as ISEST/Minimax24 campaign (http://solar.gmu.edu/heliophysics/
index.php/The_ISEST_Event_List) for Earth-affecting solar transients, ICSOM campaign(http://pansy.eps.s.u-tokyo.ac.jp/icsom/) for interhemispheric coupling during stratosphericsudden warming, and ERG-ground campaign for the dynamics of inner magnetosphere. We havesupported more than ten VarSITI-related meetings and several campaign and database
constructions every year using the SCOSTEP/VarSITI grants. VarSITI mailing list, whichcontains ~900 mail addresses from ~70 countries, was constructed for communications amongscientists on various fields. VarSITI newsletters have been published every three months tointroduce new scientific results, young scientists newly joined into the VarSITI science, andmeeting reports. About 130 databases are registered for VarSITI-related research activities. All
this information is available at the VarSITI web pages at http://www.varsiti.org/. After the first
three years of the VarSITI program, various outstanding results has been obtained, such as solar
dynamo simulations, imaging measurements of earth-affecting solar transients, high-energy
particle precipitation on the Earth’s atmosphere and its consequence on the ozone and otherconstituents in the upper and middle atmosphere, and effects of lower atmosphere to thethermosphere and ionosphere through the middle atmosphere. In the presentation we will review
these various recent results obtained during the VarSITI period.
VARIABILITY OF THE X-RAY SUN FROM THE SOLAR ATMOSPHERE
Zavkiddin Mirtoshev
Samarkand State University, Samarkand, Uzbekistan
zmirtoshev@gmail.com

I have analyzed the time series of full disk integrated soft and hard X-ray emission fromthe solar corona during 2004 January 1 to 2009 December 31, covering the descending phase ofsolar cycle 23 from global point of view. I employed the daily X-ray index (DXI) derived from
X-ray observations from the “Solar X-ray Spectrometer” (SOXS) mission in three different
energy bands: 4–5.5 keV (soft X-rays) and 15–20; 20–25 keV (hard X-rays). The application ofLomb–Scargle periodogram technique to the DXI time series observed by the Si detector in theenergy bands reveals several short- and intermediate-periodicities of the X-ray corona. The DXI
explicitly show the periods of ~13.6 days, ~26.7 days, ~128.5 days, ~151 days, ~180 days, ~220
days, ~270 days, ~1.24 year and ~1.54 year periods in soft X-ray as well as in hard X-ray energy
bands. Although all periods are above 70 % confidence level in all energy bands, they show
strong power in hard X-ray emission in comparison to soft X-ray emission in accordance to
Chowdhury et al. These periods are explicitly clear in all energy bands. The flare activity Rieger
periods of ∼150 and 180 and near Rieger period of ~220 days are very strong in hard X-ray
emission, which is very much expected. On the other hand, our current study reveals strong 270day periodicity in soft X-ray emission, which may be connected with tachocline, similar to
fundamental rotation period of the Sun. The 1.24-year and 1.54-year periodicity observed frommy research work is well observed in both soft as well as in hard X-ray channels. These longterm periodicities must also have connection with tachocline and should be regarded as aconsequence of variation in rotational modulation over long time scales. I gratefully
acknowledge support by the Indian Centre for Space Science and Technology Education in Asiaand the Pacific (CSSTEAP, the Centre is affiliated to the United Nations), Physical ResearchLaboratory (PRL) at Ahmedabad, India. This work has done under the supervision of Prof.
Rajmal Jain and paper consist materials of pilot project and research part of the M. Tech program
which was made during Space and Atmospheric Science Course.
33

CONTRIBUTION OF TSI, SOLAR UV AND ENERGETIC PARTICLES TO EARLY
20TH CENTURY CLIMATE AND OZONE LAYER EVOLUTION
Eugene Rozanov
PMOD/WRC and IAC ETHZ, Switzerland
eugene.rozanov@pmodwrc.ch

The early 20th century warming is visible in several observation data sets but themechanisms causing this phenomenon remain unclear. During this period the climate systembehavior was controlled by the increase of greenhouse gases, recovery after preceding
volcanically active period, steady increase of solar magnetic activity. The former presumably
leads to increase of solar irradiance and geomagnetic activity followed by more intensive
energetic electron precipitation and decrease of ionization by galactic cosmic rays. To elucidate
the role of different anthropogenic and natural forcing we performed several atmosphere-ocean
chemistry-climate model (AOCCM) SOCOL-MPIOM runs driven by different combinations offorcing. In this talk we will compare the contributions of energetic particles and solar irradiance.
The ionization rates and influx of NOx from the thermosphere were taken from the dataset
prepared for IPCC CMIP-6. The solar irradiance time series was reconstructed from the solar
modulation potential and sunspots time series. The obtained model results allow estimating themain drivers of climate and ozone changes in the first half of the 20th century. Preliminary
results showed that the contribution of energetic particles is more important for the surface
climate over the northern landmasses than solar UV, but over the oceans the contribution fromthe visible and infrared solar irradiances dominates. We show that the treatment of energetic
particles leads to better agreement of the simulated surface air temperature trends over Europe
and Eastern US with observations. The comparison of the simulated and observed total ozone
evolution will be also discussed.

MODERN DALTON MINIMUM AND DISASTER RISK ON CLIMATE CHANGE
Ahmed Abdel AbdelHady
Astronomy, Space and Meteorology Dept. Faculty of Sciences, Cairo University, Egypt
aahady@sci.cu.edu.eg

The global warming caused by the green-house gases effect will be equal or less than the
global cooling as a result of the current era of weak solar activity. In this respect, we refer to theModern Dalton Minimum (MDM), according to which the earth’s surface temperature will
become cooler than nowadays, starting from the year 2005 until the year 2050. However, thedegree of cooling, previously mentioned in old Dalton Minimum (c. 210 y ago), will beminimized by building-up of green-house gases effect during the MDM period. Regarding to theperiodicities of solar activities, it is clear that now we have a new solar cycle of around 210 years.
This paper analyses solar-X activity data given by GOES satellite to predict the incoming effectsof the MDM on the climate change, global precipitation and the change of dryland areas all overthe Earth surface.

34

TIME AND SPATIAL PATTERNS OF SOLAR VARIABILITY INFLUENCE ON THE
EARTH’S CLIMATE
Alexander Ruzmaikin, Joan Feynman
Jet Propulsion Laboratory, California Institute of Technology, United States
alexander.ruzmaikin@jpl.nasa.gov

One of the potential contributors to the climate change is solar activity variability
associated with the low-to-high solar irradiance input to the Earth. We discuss the time andspatial patterns formed in the Earth’s climate system under the solar variability forcing on timescales from 11-year solar cycle to the centennial solar variability such as the Centennial
Gleissberg Cycle (CGC), a 90–100 year variation of the amplitude of the 11-year sunspot cycle
observed on the Sun, solar wind, and at the Earth using the Total and Spectral Solar Irradiances
reconstructed for over three centuries. The Earth’s climate response to the prolonged low solar
irradiance involves heat transfer to the deep ocean with a time lag longer than a decade. We
identify the timing and spatial pattern of the Earth’s climate response that allows distinguishing thesolar forcing from other climate forcing and discuss the spatial and time correlation of the patterns
induced by solar forcing with the naturally formed climate patterns such as NAM, PNA and PDO.

PROGRESS IN LONG-TERM TRENDS IN THE MLT REGIONJan Lastovicka1, ROSMIC WG3 Team2
1

Institute of Atmospheric Physics, Czech Academy of Sciences Bocni II, 14131 Prague, Czech
Republic,
2
Worldwide Team, Germany

The increasing atmospheric concentration of greenhouse gases results in long-term changes
not only in the troposphere; it affects also the mesosphere and lower thermosphere (MLT) andthe embedded part of the ionosphere. Progress in investigating long-term trends in the MLT
region will briefly be reviewed. There are also secondary trend drivers like ozone, geomagnetic
and solar activity, atmospheric waves coming from below, and water vapor. Their unstablebehavior makes the investigation of trends more difficult and trends themselves less stable.
Among important areas of progress we may include the first satellite observations of carbon
dioxide trends in the MLT region, better understanding and simulation of the observed impact ofozone on trends, substantially better agreement of most recent model simulations of trends withobservations, better knowledge and simulation of trends in polar mesospheric clouds, and someother results to be presented in the talk.

35

FORMATION OF POLAR CORONAL HOLES IN CYCLE 24
Elena Golubeva, Alexander Mordvinov
Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
golubeva@iszf.irk.ru

Asynchronous reversal of the Sun’s polar fields in the current cycle and asymmetry in theformation of polar coronal holes are studied. A stable coronal hole was first formed at the South
Pole, despite the later polar-field reversal there. On the basis of a synoptic map analysis, westudy causal relationships between decay of activity complexes, evolution of large-scale
magnetic fields, and formation of coronal holes. Ensembles of coronal holes are usuallyassociated with decaying activity complexes. After the polar-field reversals, the Sun’s open
magnetic flux rearranges globally. During this period, ensembles of coronal holes interact withactivity complexes, forming trans-equatorial corridors through which the open magnetic flux
redistributes between the hemispheres. High-latitude ensembles merge with polar coronal holes,
increasing their areas until the end of a cycle. Analysis of cause-and-effect relationships showedthat the south polar coronal hole was formed from coronal holes originated after the decay ofmultiple activity complexes observed during 2014. High-latitude unipolar magnetic regions of
opposite polarities resulted in a complicated magnetic configuration in the northern polar zone.
This delayed formation of the polar coronal hole for 1.5 year. During the declining phase of thecurrent cycle, the stable polar coronal holes formed extensions that reached opposite
hemispheres. Despite low sunspot activity in the current cycle, these huge coronal holes
produced solar wind streams, which led to recurrent geomagnetic storms.
THE SUN’S POLAR-FIELD REVERSAL IN THE CURRENT CYCLE: THE EFFECTS
OF NORTH-SOUTH ASYMMETRY OF SUNSPOT ACTIVITY
Alexander Mordvinov1, Alexei Pevtsov2
1
2

Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
National Solar Observatory, Sunspot, NM, United States

avm@iszf.irk.ru

In order to study the Sun’s polar-field reversal, we analyzed synoptic data from the Vector
Stokes Magnetograph (VSM) of Synoptic Optical Long-term Investigations of the Sun (SOLIS)
and the NASA SDO/HMI facility. Development of solar activity in the current cycle made it
evident that the North–South asymmetry of sunspot activity resulted in an asynchronous reversalof the Sun’s polar field. The decay of activity complexes in late 2011 and 2014 were of crucial
importance for the polar-field reversals at the northern and southern poles. After decay ofmultiple activity complexes, the surges of trailing polarities reached the Sun’s poles and led tothe polar field reversals. Then two leading-polarity surges reached the northern polar zone andled to mixing of magnetic polarities there. The leading-polarity surges originated due to lowlatitude magnetic bipoles, which are characterized by negative tilt angles contrary to Joy’s law.
The north-south asymmetry also appears in the polar-flux imbalance. Unlike the southern polar
zone, the flux imbalance near the North Pole shows no cyclic changes and varies about zero.
Such polar-flux imbalance reveals one more peculiarity of the current cycle. Amplitude ofcumulative flux imbalance at the North Pole is less by factor of five as compared to that at theSouth Pole. The unusual behavior of the imbalance is caused by low sunspot activity and theviolations of Joy’s law, which resulted in weak polar field of mixed polarities near the North Pole.
36

LONG-TERM RELATIONSHIP BETWEEN DOMINANT IMF SECTOR STRUCTURE
AND IONOSPHERE VARIABILITY
Tamara Gulyaeva, Ljubov Poustovalova
Pushkov Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation RAS,
Moscow, Russia
gulyaeva@izmiran.ru

IMF Bz component serves as a crucial factor to understand the IMF sector related solarterrestrial phenomena since the solar wind energy transfer into the magnetosphere is favored by
the negative IMF Bz component (towards the Earth) and resisted by the positive Bz component(towards the Sun). In this study, the perturbations of the ionospheric critical frequency, foF2, at
Moscow are analyzed regarding the IMF Sector Structure (IMF-SS), specified by the Leif
Svalgaard’s list of sector boundaries (http://www.leif.org/research/sblist.txt) and the half-day
dominant sign of Bz retrieved from the polar geomagnetic observations (http://www.izmiran.ru/
stp/polar/SSIMF/). The half-day IMF-SS is estimated from the magnetometer measurements at
Churchill and Vostok observatories where the polar diurnal geomagnetic variations serve as aproxy of sign of Bz for the IMF sector surrounding the Earth (Mansurov and Mansurova, 1970;
Svalgaard, 1976). The long-term IMF-SS characteristics for 1958–2017 show dominant positive
Bz > 0 (towards the Sun) half-day periods as compared to Bz < 0 with this trend growing from the19th to 24th solar cycles. Relevant Catalogue of foF2 disturbances at Moscow(http://www.izmiran.ru/ionosphere/weather/dat5/dist_mos.txt) is analyzed for the positive andnegative IMF Bz during the 23rd-24th solar cycles demonstrating association of the mid-latitude
ionosphere variability with the IMF-SS sector structure.

IMPACT OF EPP AND GCRs ON ATMOSPHERIC ELECTRIC CIRCUITAND CLIMATE
Irina Mironova
St. Petersburg State University, St. Petersburg, Russia
irini.mironova@gmail.com

The summary and progress on the topic “Direct and Indirect Impact of energetic particle
precipitation (EPP), galactic cosmic rays (GCRs) and Electric Circuit on Climate” will bepresented here. The overview of the main advances will cover subjects defined as:- Observations of energetic particles in the Earth atmosphere;- Atmospheric ionization by energetic particle precipitation;- Impact of EPP and GCRs on the Global Electric Circuit;- Definition of energetic particles inputs for climate modeling;- Impact of energetic particles on climate.
Finally open questions and summary coming out will be presented as a conclusion.

37

INTENSE GEOMAGNETIC STORM EFFECTS ON THE NORTH ATLANTICOSCILLATION
Gerardo L. Flores Ivaldi1, Ana G. Elias2,3, Marta Zossi2,3, Teresita Heredia3
1

Departamento de Fisica, Facultad de Ciencias Exactas y Tecnologia, Universidad Nacional de
Tucuman, Argentina
2
CONICET, Argentina
3
FACET-UNT, Argentina
gerflores@hotmail.com

Considering the solar activity level, the association between short-term variability in the
North Atlantic Oscillation (NAO) and intense geomagnetic storms is analyzed using daily data
records. The NAO, being the dominant pattern of variation in atmospheric circulation in the
North Atlantic basin, results in a large-scale modulation of the normal patterns of heat andmoisture transport especially in winter. It determines changes in temperature and precipitation ina great area from eastern North America to Central Europe. A positive correlation between longterm variations in several studies the NAO and geomagnetic activity has already been shown inseveral studies. However, at daily timescales, from the study of more than 200 geomagnetic
storms we observe a decrease in the NAO index coincident with the maximum intensity of thegeomagnetic storm. An explanation of our results is given through the upper atmosphereprocesses induced by geomagnetic storms followed by coupling mechanisms among the different
atmosphere regions, reaching finally the troposphere, in the context of an overall increasing trend
which may be due to anthropogenic activity. A possible explanation would be that the NAO
decrease due to geomagnetic storms is highly localized in time at daily scales and the highpositive correlation between geomagnetic activity indices and NAO, especially after 1970, is due
merely to a coincidence of increasing trends in both parameters.
NORTH ATLANTIC OSCILLATION VARIABILITY LINKED TO THE AURORALELECTROJET INDEX, AE
Gerardo L. Flores Ivaldi1, Marta Zossi2,3, Teresita Heredia3
1

Departamento de Fisica, Facultad de Ciencias Exactas y Tecnologia, Universidad Nacional de
Tucuman, Argentina
2
CONICET, Argentina
3
FACET-UNT, Argentina
gerflores@hotmail.com
The possible association between the North Atlantic Oscillation (NAO) variability and the auroralelectrojet index, AE, is analyzed. The NAO is the dominant pattern of variation in atmospheric circulationin the North Atlantic basin. This oscillation results in a large-scale modulation of the normal patterns ofheat and moisture transport, especially in winter, which determines changes in temperature andprecipitation in a great area from eastern North America to Central Europe. A positive
correlation between long-term variations in the NAO and geomagnetic activity has already beenshown in several studies, using the aa index. In the present work, the AE index is used instead,which monitors the auroral electrojets in the Northern hemisphere (a measure of global electrojet
activity in the auroral zone). An explanation of our result is given through the upper atmosphereprocesses induced by geomagnetic storms followed by coupling mechanisms among the different
atmosphere regions, reaching finally the troposphere, in the context of an overall increasing trend
which may be due to anthropogenic activity.
38

SUNSPOT NUMBER: THE ONGOING MODERNIZATION OF A LONG-TERM
REFERENCE
Frédéric Clette, Laure Lefèvre
Royal Observatory of Belgium, Brussels, Belgium
frederic.clette@oma.be

Since July 2015, a new entirely recalibrated version of the sunspot number series (Version 2.0)
has replaced the original static record of past solar activity (http://sidc.be/silso). The simpler but
longer group number series was also updated, leading to two main multi-century reconstructions.
This also marked a fundamental transition towards a continuous research-driven upgrading
process, equivalent to other modern astronomical standards like the total solar irradiance. After
presenting the changes introduced to the original series, we discuss the remaining inconsistencies
between the sunspot and group number series published over recent months. Although the main
inhomogeneities are now established and corrected (drifts and jumps around 1885 and 1947 andafter 1981), several inconsistencies and uncertainties remain. In particular, the early part of theseries before 1826 suffers from larger uncertainties and also from the scarcity of data over a few
critical time intervals. New more advanced statistical methods, like non-linear regression or renormalization, are also introduced to replace the past classical mean k ratios for normalizing thedata from individual observers. In order to continue this work, a coordinated effort was initiatedin 2017 and will be articulated around several thematic working groups and a cycle of dedicatedworkshops. We conclude on the current early progresses of these expert groups and we outline
the key advances to be expected in the upcoming new update of the sunspot record (Version 3.0)
and the possible implications for solar and solar-terrestrial research.

EXTREME SOLAR EVENTS: DEBATE ON VALIDITY, ORIGIN AND PROPERTIES
Leonty Miroshnichenko1,2
1

Pushkov Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation RAS,
Moscow, Russia
2
Skobeltsyn Institute of Nuclear Physics, Lomonosov Moscow State University (SINP MSU),
Moscow, Russia
leonty1937@mail.ru

Modern concept of Extreme Solar Event (ESE) is critically analyzed based on available
direct and proxy data on solar cosmic rays (SCR), or solar energetic particles (SEP). Special
attention is paid to recent debate on validity, origin and properties of the events AD775 andAD1859 (Carrington event). We demonstrate that, in spite of existing uncertainties in proton
fluences above 30 MeV, all of them are fitted well by a unique distribution function, at least,
with present level of solar activity. Extremely large SEP fluxes are shown to obey a probabilistic
distribution with a sharp break in the range of large fluences (or low probabilities). The studiesof this kind may be extended for the periods with different levels of solar activity in the pastand/or in the future. Considering the recent confirmation of super-flares on solar-type stars, thisissue merits attention.

39

SOLAR VARIABILITY MANIFESTATIONS IN WEATHER AND CLIMATIC
CHARACTERISTICS
Geliy Zherebtsov, Vladimir Kovalenko, Sergey Molodykh, Kiril Kirichenko
Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
sim@iszf.irk.ru

Studies of solar activity influence on weather and climate has got a long history.
Nevertheless, the question of whether solar activity contributes significantly to weather andclimate change is still debatable. We discussed the main physical processes responsible forclimate changes in the 20th century, and the issues that are of primary importance forunderstanding the nature of these changes. Most papers dealing with study of SA possible
contribution to changes in climatic characteristics, consider the solar constant (SC) as the solar
activity (SA) index in. However, SC changes (0.1 %) cannot contribute much to the observed
global temperature variations. The ISTP proposed another mechanism of the SA influence on the
climate and developed a physical model. The model key concept is the SA influence on the
Earth’s climate system parameters controlling the outgoing long-wave radiation in high-latitude
regions. According to measurements of the atmospheric electricity parameters during
geomagnetic disturbances, as well as during invasion of large fluxes of solar cosmic rays in polar
latitudes, there is a significant increase in the tropospheric electric field and the ionosphere—
Earth current. Changes in the electric field exert influence on vertical distribution of charged
aerosols, which are the condensation nuclei and, hence, may affect the conditions of cloudformation and radiation balance in high-latitude regions. Hereby, there are changes in thethermobaric field of the troposphere, and in meridional temperature gradient, determining themeridional heat transport. As a result, the Earth’s climate system heat content and the global
climate are changing. We present and discuss the results of analysis of regularities and featuresof the troposphere and sea surface temperature reactions both to some heliogeophysicaldisturbances, and to long-term changes in solar and geomagnetic activity. New proofs of solar
activity influence on climate processes in the ocean and troposphere are found. We revealed a
reliable response to the SA influence in the main climatic characteristics: surface temperature,sea surface temperature, and precipitation. It has been determined that the climatic response to
the solar and geomagnetic activity is characterized by significant space-time irregularity; theresponse is regional and depends on the general circulation of atmosphere. We showed that SA
contributed significantly to the global climate change basically during the first warming period in
the 20th century (1910–1943). This period is characterized by a significant positive trend in thelevel of geomagnetic activity; the activity was the highest over the entire period considered(1868–2015), which matched the increased meridional heat transport in the North Atlantics.

40

SPACE CLIMATE IN THE HELIOSPHERE-MAGNETOSPHERE ENVIRONMENT.
CONSEQUENCES IN SOLAR CYCLE 24
Venera Dobrica, Crisan Demetrescu, Cristiana Stefan
Institute of Geodynamics, Romanian Academy, Bucharest, Romania
venera@geodin.roSpace climate characterizes long-term variability in the heliosphere-magnetosphereenvironment. Our previous studies showed that the parameters describing this environment
evolved at timescales related to the magnetic (Hale) solar cycle and to Gleissberg solar cycle.
In this study we use the Hodrick-Prescott (HP) and Butterworth filtering to get the long-term
variations, at inter-decadal (22 years) and sub-centennial (80-90 years) timescales, in several
heliospheric (heliospheric magnetic field intensity, solar wind speed), and magnetospheric(geomagnetic indices which describe electric current systems in the magnetosphere or ionosphereand the variable geomagnetic field with external sources given by COV-OBS.x1 geomagnetic
model) parameters. We show that the actual trend in space climate is given by the superposition of
the inter-decadal and sub-centennial variations on the long-term inter-centennial trend.

INVESTIGATION OF SEASONAL TREND ANOMALIES IN MIDLATITUDE
IONOSPHERE USING DROT
Feza Arikan1, Emre Efendi1, Ali Cinar2, Secil Karatay2
1
2

Hacettepe University, Turkey
Kastamonu University, Turkey

arikan@hacettepe.edu.tr

Solar radiation is the most dominant contributor of ionospheric trend in diurnal, seasonal,
annual and 11-year cycles. Seasonal variability can deviate from expected trends with
disturbances named as anomalies. Total Electron Content (TEC) is one of the most commonlyused observables of ionospheric variability. TEC can be estimated from worldwide dual
frequency Global Positioning System (GPS) receivers which allow a dense representation oftrend anomalies in midlatitude regions. Differential Rate Of TEC (DROT) is a promising method
in detection of disturbances. DROT method is based on the ratio of smoothed detrended
derivative of TEC to low-pass filtered Rate Of TEC (ROT). Typically, for 40 % < DROT <55 %,minor and singular disturbances can be present. For 55 % < DROT <75%, moderate disturbances
can be observed. DROT values that are larger than 75 % are indicators of severe disturbancesand extreme deviations from typical diurnal trend of TEC. In this study, DROT is applied to anumber of GPS stations located in mid-latitude regions of Northern and Southern hemispheres
during 23rd and 24th solar cycles. It is observed that the value of TEC increases during solar
active years, and the amplitude of deviation becomes less significant. During solar minimum
years, the variability in TEC due to activities other than solar variability becomes dominant.
Thus, the typical annual average value is around 55 % to 60% (moderate) for a solar maximum
year, whereas the same value rises to 75 % for a solar minimum year. The highest values areobserved during winter (summer) months for Northern (Southern) Hemisphere. DROT values
start to decrease after Spring (Autumn) Equinox for Northern (Southern) Hemisphere and reachto a local minimum during April and May (October and November) for Northern (Southern)
41

Hemisphere. An increasing (decreasing) trend is observed after November where a maximum(minimum) is reached with December for Northern (Southern) Hemisphere. Deviations from theexpected diurnal behavior of TEC such as winter night time anomalies or bite-out phenomena
increase the value of DROT to moderate and severe disturbance levels that can last for a numberof consecutive days. Therefore, it can be concluded that DROT can serve as an indicator of
deviation from the diurnal trend due to seasonal variability and it can also help to classify thesingle event upset type disturbances such as geomagnetic storms and seismic activities.
ON THE POSSIBILITY TO PREDICT THE FUTURE SUNSPOT MAXIMUM
Boian Borissov Kirov1, Katya Yancheva Georgieva1,Vladimir Obridko2
1

Space Research and Technology Institute BAS, Sofia, Bulgaria
Pushkov Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation RAS,
Moscow, Russia
2bkirov@space.bas.bg

The influence of solar activity on the Earth’s magnetic field has been studied for many
years. It was found that there are two main factors causing geomagnetic storms: coronal massejections whose probability is proportional to the number of sunspots, and high speed solar windstreams. As the times of the sunspot maximum and the high speed solar wind streams maximum
do not coincide, there are two geomagnetic activity maxima in each 11-year solar cycle. In thepresent work we regard the Earth as a probe immersed in the solar wind, and based on the data
for the time interval between the sunspot maximum and the geomagnetic activity maximum inthe declining phase of the sunspot cycle n, and the value of the minimum geomagnetic activity inthe beginning of sunspot cycle n+1, we forecast the maximum of cycle n+1.

LONG TERM VARIATIONS IN THE RATIO BETWEEN THE NUMBER
OF SUNSPOTS AND THE NUMBER OF SUNSPOT GROUPS
Katya Georgieva1, Ali Kilcik2, Yuri Nagovitsyn3, Boian Kirov1
1

Space Research and Technology Institute BAS, Sofia, Bulgaria
Akdeniz University, Department of Space Science and Technologies, Antalya, Turkey
3
Central Astronomical Observatory at Pulkovo, St. Petersburg, Russia
2katyageorgieva@msn.com

The sunspots are the most obvious manifestation of solar activity, and the one with thelongest instrumental data record. Until very recently, two indices were used to quantify thesunspot activity: the Zurich International sunspot number introduced by Wolf, based on thenumber of the observed individual sunspots and the number of sunspot groups, and the Groupsunspot number, based solely on the number of the observed sunspot groups. The long-term
variations of these two indices diverge, which can be either a manifestation of variations in theoperation of the solar dynamo, leading to variations in the average number of sunspots per
sunspot group, or an artifact of changes in observers, pilot observatories, instruments,
observational routines, calculation schemes, etc. We use data from three observatories with
continuous and homogeneous data to study this problem.
42

VARIATIONS OF THE SOLAR SPECTRUM IRRADIANCE IN THE VISIBLE
AS OBSERVED WITH SOLAR/SOLSPEC DURING CYCLE 24
Abdanour Irbah1, Luc Damé1, Slimane Bekki1, Mustapha Meftah1, David Bolsée2,
Nuno Pereira2
1
2

LATMOS / CNRS /UVSQ /UPMCGUYANCOURT, France
BIRA-IASB, Belgium

air@latmos.ipsl.fr

The solar spectral irradiance (SSI) and its temporal variations are of prime importance toapprehend the physics of the Sun and to understand its effects on Earth climate through changesof atmospheric properties. Ground based measurements of SSI are indeed affected by the Earthatmosphere; space observations are therefore required to perform adequate observations. Only a
few long series of SSI space measurements were obtained these last decades. The SOLSPEC
instrument of the SOLAR payload on the International Space Station (ISS) has recorded one ofthem from April 2008 to February 2017 (last measurements the 15th) covering almost the wholesolar cycle 24. The instrument is a spectro-radiometer recording data of the Sun from 166 to
3088 nm. Operated from the ISS in a harsh environment, it needed appropriate processing
methods to extract significant scientific results from noise and instrumental effects. We present
the original methods used to process the data to evidence visible SSI variations during cycle 24.
We then discuss the results obtained showing SSI variations in phase with solar activity.

PROPERTIES OF FILAMENTS IN SOLAR ACTIVITY CYCLES N 15–24
Kseniya Tlatova1, Valeriya Vasil’eva2, Andrey Tlatov1,2
1

Kislovodsk Mountain Astronomical Station of the Pulkovo Observatory, Russia
Kalmyk State University, Elista, Russia
3
Kislovodsk mountain astronomical station of the Pulkovo observatory, Russia
2

k.tlatova@mail.ru

The series of solar filaments characteristics is represented. This series is obtained byprocessing of daily observations in the H-alpha line according to the Kodaikanal observatory in
Kodaikanal (India, 1912–2002). The series is complemented by database of filaments properties
according to Kislovodsk for the period 1959–2016, Sacramento Peak (USA, 1962–2002) andMeudon (France, 1982–2015). These data are unique because they trace the polarity inversion
line which helps to identify the large-scale organization of the solar magnetic field. To selectsolar filaments boundaries, we have developed methods based on automatic allocation
procedures of low-contrast objects on the solar disk, and methods of editing the selectedstructures in semi-automatic mode. More than 24 thousand photographic plates were processedin total for Kodaikanal with more than 326 thousand filaments being allocated. Comparative
analysis of solar filaments characteristics in 15–24 cycles of activity was carried out. The
connection of solar filaments indices and long-term parameters of space weather is considered.

43

RADIO EMISSION OF ACTIVITY COMPLEXES ON THE SUN IN
mm- AND cm- WAVES
Anastasia Vidrenkova
Department of Theoretical Physics and Astronomy of Odessa I.I. Mechnikov National University,
Ukrainecool.vidrenkova@yandex.ua

Activity complexes (CA) and complexes of active regions (CAR) on the Sun are among
the largest scales in the manifestation of solar activity. Here are the most powerfulmanifestations of solar activity as a result of the interaction of various cores of activity inside thecomplex. Currently they are defined according to the data of сosmic orbiting solar observatories
SOHO and SDO by UV and x-ray radiation in the corona. Radio maps of the Sun on millimeterand centimeter wavelengths allow the identification of CAO and CA and at lower levels in thechromosphere and the corona. This allows to connect a manifestation of activity from underphotosphere levels convection zone to magnetosphere complexes in the solar chromosphere andCorona. In this paper, the technique of identifying complexes is presented and the dynamics oftheir activity in radio emission according to observation data of stations of the international Sun radio
service KRIM: RT-22, RT-2, RT-3, PT-m (since 1957) in the Department of radio astronomy andGeodynamics of the Crimean Astrophysical Observatory, Metsahovi Radio Astronomy Observatory
on RT-14 (37 GHz), Radioheliographs Nobeyama(17 and 34 GHz) and SSRT (Irkutsk, 5.1 GHz). A
feature of these data is that they allow to explore the dynamics of development of activity complexes
from the 20th activity cycle when space observatories have not worked yet.
HURRICANES OVER ATLANTIC REGION DURING 1851–2010
AND SOLAR INFLUENCE ON IT
Dhruba Banerjee
Faculty Member, Swami Vivekananda Institute of Science and Technology, Dakshin Gobindapur,
Kolkata-700145, India
dhrubabanerjee81@gmail.com

The analysis of hurricane frequency during 1851–2010 reveals (1) It increases
monotonically from 1851 up to 1910, then it begins to decrease slowly (2) Monthly variation
also exists namely, the frequency is much more during august to October, September being themonth of maximum Hurricane. The reverse is the situation during December to June. The 30
years variation study shows that in 1941–1970 and 1971–2000 total hurricane were maximum.
The analyse of the rates of change of frequency shows that the rate monotonically increases since1851 the max. Being during 1971–2000 (1.22 per yr. approx.). But after that it began to decrease.
Another very interesting aspect is that the frequency of hurricane is found to decrease .When
Solar activities are increased i.e. when Sun’s Spot Number increases calculate the decadalfrequency study shows that from it was less than 10 before 1991 but more than 10 after 1991 andduring 2001–2010 it was 13.3. A very striking feature is that the average frequency over the timeof solar maxima is 8.3 which is less than the normal average (8.8) but average over solar minima
years is (9.53). Evidently, these suggest adverse effect of solar activities on hurricane formation.
This is similar to the resistance found in cyclone formation. Possibly the solar hot material
produces this resistance to the formation of hurricane/cyclone.

44

SCIENTIFIC HIGHLIGHTS FROM ROMIC
Franz-Josef Lübken
Leibniz Institute of Atmospheric Physics, Kühlungsborn, Germany
luebken@iap-kborn.de

The German Federal Ministry of Education and Research (Bundesministerium fur Bildung
und Forschung, BMBF) has launched a research initiative in 2013/2014 called ROMIC (Role ofthe Middle Atmosphere in Climate). The aim of ROMIC is to improve our understanding of longterm variations in the stratosphere, mesosphere, and lower thermosphere and to investigate theirpotential role for climate changes in the troposphere. This includes to study couplingmechanisms between various layers and the relative importance of anthropogenic and naturalforcing, e.g., by the Sun. Scientists at a total of 15 research institutes in Germany are involved
and cover a large range of experimental and theoretical topics relevant for ROMIC. Some
scientific highlights from the research projects within ROMIC will be presented.

ANALYSIS OF VARIATIONS OF EARTH’S MAGNETIC FIELD PRODUCEDBY EQUATORIAL ELECTROJETS IN SUDAMERICA
Franklin Bolívar Aldás
Quito Astronomical Observatory, National Polytechnic School, Quito, Ecuador
franklinaldas@hotmail.com

Observations of the magnetic field in Huancayo in 1922 demonstrated the existence of theEquatorial electro jets, which is a narrow band of electrons traveling east to west 180 km above
the Earth’s surface by a belt along dip equator. Wind-driven currents, through the dynamo
mechanism, produce an accumulation of positive charges at sunrise and negative at sunset, whichtranslates into considerable variations in the geomagnetic field. In this study, we have used theEarth magnetic field (MG) data provided by Jerusalem station located in Ecuador, above thegeographic equatorial line, in order to study its secular variation founding an strong correlation
with sunspots number which indicates the influence of solar activity on the Earth’s ionosphere.
We also have used the magnetic field data from others 5 magnetic stations in order to study forfirst time the latitudinal dependence of the EEJ current and its morphological features in
SudAmerica. We have found that the average electrojet current is symmetrically distributed
along 25 degrees around the position of the peak of intensity, so that the jet extends from -10 To
15 degrees in magnetic latitude and the maximum intensity measured experimentally was in thestation of Huancayo by its proximity with the dip equator.

45

THE LARGE SYMMETRIC SUNSPOT GROUPS AS POSTDICTORS OF ACTIVELONGITUDES AT THE SUN DISC
Alexey Rybak
Central Astronomical Observatory of RAS at Pulkovo, St. Petersburg, Russia
solarfish@alexeyryback.ru

This paper considers a longitude distribution of sunspot groups over 1982–2015, using datafrom the National Geophysical Data Center (Boulder, USA). The space-time distribution ofsunspot groups is analyzed in coordinate sectors calculated from heliographic longitudes of thegroups. A longitude extent of a coordinate sector is compared to the average size of one active
region (30–40°). Then, in each coordinate sector, evolutionary activity of sunspot groups issummarized according to classification values after Malde (CV) throughout the observation
period. The longitude distribution of large sunspot groups plotted in such a way does not reveal
anticorrelation between Northern and Southern hemispheres in sunspot cycle 23. More than five
thousand large symmetric sunspot groups of the Boulder classifications CHO, DHO, EHO, FHO
and HHX have been detected under the NGDC program. The average CV (43.72±4.44), theaverage number of sunspots in a group (6.54±7.10), and the average total area of groups(278±207 millionths of a solar hemisphere) suggest that the first of the listed indices allows us toconsider simple groups with a large symmetric sunspot as postdictors of the intense process ofsunspot formation in previous solar rotations. Consequently, we can analyze the statistics onlongitude-time distribution of groups of large sunspots, using average CV for such a sunspot class.

SOLAR CYCLE PREDICTIONS AND PREDICTABILITY
Robert Harold Cameron
Max Planck Institute for Solar System Research, Göttingen, Germany
cameron@mps.mpg.de

How strong will the next solar cycle be? The one after that? How certain are we in ouranswers?In this talk I will review some previous work aimed at answering these questions andwhy the problem is difficult. Infernces based on high-resolution observations of today, sunspot
drawings up to 400 years old, isotope records going back about 10000 years and stellar
observations will be combined in an attempt to come to a conclusion.

46

THE EXPECTED FLUXES OBSERVED BY STIX DURING DEEP MINIMUM
OF SOLAR ACTIVITY
Magdalena Gryciuk1,2, Tomasz Mrozek1,2, Marek Siarkowski3, Marek Stęślicki3
1

Space Research Centre of Polish Academy of Sciences, Solar Physics Division, Poland
Astronomical Institute, University of Wroclaw, Poland
3Space Research Centre of Polish Academy of Sciences, Solar Physics Division, Poland2

mg@cbk.pan.wroc.pl

The Spectrometer Telescope for Imaging X-rays (STIX) installed onboard Solar Orbiter
mission will be launched in the autumn 2018. The instrument is designed for imaging andspectroscopy of solar X-ray sources in the energy range 4-150 keV. After three years of cruise phase
it will start to gather scientific data from the orbit with perihelion distance about 0.3 AU. The firstscientific phase of the mission will last three years and after which extended phase of the mission is
expected. It means that STIX will operate also during the next solar minimum. For maximizing
scientific output of the instrument we have to define observing modes for every expected scenario.
Therefore we decided to estimate fluxes measured by the instrument during periods of extremely low
solar activity. For this purpose we used real measurements which were conducted by the Solar
Photometer in X-rays (SphinX), instrument designed to observe soft X-ray solar emission in theenergy range between 1.2 keV and 15 keV with the resolution better than 0.5 keV. The SphinX
operated from February until November 2009 aboard CORONAS-Photon satellite, during thephase of exceptionally low minimum of solar activity. Despite a very low activity about 1600
small X-ray events have been recognized by semi-automatic inspection of SphinX light curves.
Many of them were registered above 4 keV STIX threshold. With a use of SphinX data we wereable to estimate fluxes that will be observed by STIX during a period of low solar activity anddefine the observational modes which will allow us to gather valuable spectra and effective
image reconstruction.
SOLAR/SOLSPEC 9 YEARS OF SOLAR SPECTRAL IRRADIANCE FROM SPACE:
NEW REFERENCE SPECTRA IN UV AND IR, AND VARIABILITY RESULTS
Luc Damé1, Mustapha Meftah1, David Bolsée2, Nuno Pereira2, Abdenour Irbah1,
Slimane Bekki1, Alain Hauchecorne1, Dominique Sluse2, Gaël Cessateur2
1
2

LATMOS/IPSL/CNRS/UVSQ, Guyancourt France
BIRA-IASB, Brussels, Belgium

luc.dame@latmos.ipsl.fr

Since April 5, 2008 and until February 15, 2017, the SOLSPEC (SOLar SPECtrometer)
spectro-radiometer of the SOLAR facility on the International Space Station performed accurate
measurements of Solar Spectral Irradiance (SSI) from the far ultraviolet to the infrared (165–3088 nm). These measurements are of primary importance for a better understanding of solar
physics and of the impact of solar variability on climate (via Earth’s atmosphericphotochemistry), noticeably through the top-down mechanism amplifying ultraviolet (UV) solar
forcing effects on the climate (UV affects stratospheric dynamics and temperatures, alteringinterplanetary waves and weather patterns both poleward and downward to the lower
stratosphere and tropopause regions). SOLAR/SOLSPEC with almost 9 years of observations
covered most of the unusual solar cycle 24 from minimum in 2008 to maximum, establishing47

new reference solar spectra in UV (165–400 nm) and in infrared (656–3088 nm), thanks torevised engineering corrections, improved calibrations and advanced procedures to account forthermal, aging and pointing corrections. In addition, the quality and high sensitivity of
SOLSPEC data, allow to follow temporal variability in UV (165–400 nm) in several
wavelengths bands, in infrared and, even, in visible. Uncertainties on these measurements areevaluated and results are compared with other instruments and models.
THE FUTURE OF SOLAR SPECTRAL IRRADIANCE MEASUREMENTS
IN THE ULTRAVIOLET WITH THE SOLSIM DOUBLE-MONOCHROMATOR
Luc Damé1, Mustapha Meftah1, Abdenour Irbah1, Nicolas Rouanet1, Pierre Gilbert1,
David Bolsée2, Nuno Pereira2
1
2

LATMOS/IPSL/CNRS/UVSQ, Guyancourt, France
BIRA-IASB, Brussels, Belgium

luc.dame@latmos.ipsl.fr

Solar Spectral Irradiance (SSI) measurements in the ultraviolet (UV), and their variability,
are of prime importance to quantify the solar forcing on climate through radiation and theirinteractions with the local stratosphere, noticeably through the top-down mechanism amplifying
UV solar forcing effects on the climate (UV affects stratospheric dynamics and temperatures,
altering interplanetary waves and weather patterns both poleward and downward to the lower
stratosphere and tropopause regions). SOLSIM (SOLar Spectral Irradiance Monitor) is a newly
designed double-monochromator instrument covering the 170–340 nm ultraviolet spectral range.
It is an enhanced and optimized version of the previously flown SOLSPEC (SOLar
SPECtrometer) instrument externally mounted on the Columbus module of the International
Space Station from 2008 to early 2017. While SOLSPEC had 3 double-monochromators to cover
the UV to the infrared, the SOLSIM spectrometer is covering only the UV from 170–340 nm butwith an almost constant and higher spectral resolution (0.5 nm or better), and in within reduced
dimensions and a smaller mass (8 kg). To avoid thermal issues with the instrument, a sunsynchronous polar orbit 18h-6h at 700–750 km (for almost constant observing) is preferred to theSpace Station (SOLSIM is part of the model payload of several missions to be proposed to
CNES, ESA and NASA on small platforms). Characteristics, performances and calibrations
foreseen for this new generation SSI instrument will be presented.

LONG-TERM TRENDS IN THE MIDDLE ATMOSPHERE OBSERVEDUSING GROUND BASED AND COMBINED SATELLITE MEASUREMENTS
Venkat Ratnam
National Atmospheric Research Laboratory, Department of Space, Gadanki 517112, India
vratnam@narl.gov.in

In recent years, the middle atmosphere (10–100 km) has evoked great scientific interest as
long-term changes due to global warming can be clearly captured due to the large perturbation
amplitudes at these altitudes. We have investigated the long-term trends and variability of thestratospheric ozone, water vapor and temperature over the Indian monsoon region (IMR) using48

the long data constructed from multi satellite (Upper Atmosphere Research Satellite (UARS
MLS and HALOE, 1992–2005), Aura Microwave Limb Sounder (MLS, 2004–2015), Soundingof the Atmosphere using Broadband Emission Radiometry (SABER, 2002–2015) on board
TIMED (Thermosphere Ionosphere Mesosphere Energetics Dynamics)) observations covering
the period 1993–2015. We found a very clear regional dependence in the trends of ozone but notin the water vapor and temperature. Ozone shows an increasing trend in the lower stratosphereand decreasing above 30 km. The decreasing trend is attributed to the close association of ozone
with NOx chemistry. Temperature in the lower stratosphere shows an increasing trend, and in the
middle and upper stratosphere it shows decreasing trend. Interestingly, the altitudes of thedecreasing trend in ozone match well with the cooling trend observed in the temperature. These
results on temperature trends match well with the long-term (1998–2015) observations ofRayleigh lidar over Gadanki between 30 and 70 km. Water vapor shows an increasing trend in
the lower and middle stratosphere. This study reveals existence of strong regional dependence on
the trends. Long term zonal wind observations between 70 and 80 km over the Indian region
provided by rocketsonde (1977–1991), HRDI/UARS (1991–1999), and MST radar (1995–2015)
are used to construct a long-term data set from 1977 to 2015. Using this unprecedented data set,a decreasing trend of 2 m/s/yr is found, changing from strong eastward winds during the 1970s to
weak westward winds in recent years. On the other hand, between 80 and 98 km using medium
frequency radar observations during 1993–2009, no perceptible trend is found. Simulations of
NCAR TIME-GCM also showed a similar change in the circulation when CO2 in the atmosphere isdoubled, suggesting role of anthropogenic changes in the dynamics of the mesosphere.

LONG TERM VARIATIONS OF THE SOLAR MAGNETIC FIELDS
Aimee Ann Norton
Stanford University, Stanford, United States
aanorton@stanford.edu

The Suns variable magnetic field was documented by the mid-1800s.? Fluctuations on thesolar cycle timescale are easily seen in sunspot number, polar field strength, the butterfly
diagram, and other measures. Additional periods exist; short-term variability such as the quasibiennial variations and double-peaked maximum, and long-term variability like the ~88 year
Gleissberg Cycle and grand minima. Dynamo models have achieved some success, albeit
incomplete, in reproducing the observed behavior. However, dilemmas still exist. Is the solar
dynamo made up of three components: a near-surface one that produces small-scale magnetic
fields, a distributed one acting throughout the bulk of the convection zone, and a deep-seated one
producing strong fields in the tachocline that serve as the source for sunspots? What percentageof the flux in the interior is seen at the surface? How strongly are the hemispheres coupled andhow is that achieved? I will present a broad overview of the Suns inconstant magnetic field andthe processes considered responsible. Note that the focus will be on observations and models of
the photosphere and the solar interior.

49

NONLINEAR DYNAMO MODELS OF PRESENT AND YOUNG SOLAR ANALOGS
Valery Pipin
Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
pip@iszf.irk.ru

We show results of a comparative study of the magnetic activity for the present and young
solar analogs, which are rotating with periods of 25 and 11 days, respectively. The change of thestellar interior structure are obtained from the stellar evolution code (MESA). The model take
into account the double-cell meridional circulation structure, the solar dynamo feedback on the
global flows and effects of the non-axisymmetric magnetic field. Our results suggests that on theyoung Sun the surface latitudinal shear could be twice lesser than on the current Sun. The
magnitude of the meridional circulation at the bottom and at the top of the convection zone
remains the same for the modern and the young Sun. However, on the young solar analog themeridional circulation in the middle of the convection zone is suppressed, showing a weak triplecell pattern near the stellar equator. The young solar analog demonstrates instability for the nonaxisymmetric perturbations which can be produced by the surface magnetic activity. The
magnetic feedback on the global flows results to the long-term modulation of the magnetic
activity. On the young Sun this modulation shows the possibility for the active and inactive
branches of activity and the long cycles when the star undergoes the high activity period. We
compare our finding with results of stellar observational studies of young solar analogs.

50

Session 3: COUPLING BETWEEN THE EARTH’S ATMOSPHEREAND SPACE AND ITS RELATION TO QUIET AND ACTIVE SUN__________________________________________________________________
INFLUENCE OF METEOROLOGICAL PROCESSES ON IONOSPHEREIN EASTERN EUROPE
Olga Borchevkina1, Ivan Karpov2, Pavel Vasiliev1, Alexandra Ilminskaya1, Fedor Bessarab2
1
2

Immanuel Kant Baltic Federal University, Kaliningrad, Russia
WD IZMIRAN Immanuel Kant Baltic Federal University, Kaliningrad, Russia

opsuslova@gmail.com

We present observations of atmospheric and ionospheric parameters during strong
meteorological disturbances (storms) in the Eastern Europe. The critical frequency of the F2
layer (foF2) and the total electron content (TEC) were observed at the several stations in Eastern
Europe. The analysis of ionospheric observations has shown that during meteorological storms
the amplitude of diurnal variations in TEC decreases to 50 %; and in foF2, to 15 % as compared
to quiet days. The revealed changes in ionospheric conditions during meteorological storms are
regularly registered and represent a characteristic feature of the meteorological effect on theionosphere. Numerical experiment was made to test the hypothesis using global self-consistentmodel of the thermosphere, ionosphere and protonosphere (GSM TIP). As thermospheric sourceof disturbance was defined spatially localized moving heat source, simulating the effect of AGW
dissipation, extending the field of meteorological storm. The calculation results demonstrate thedynamics of perturbations of the upper atmosphere and ionosphere parameters caused by thesource model. The physical processes that determine the resulting ionospheric disturbances are
discussed. The characteristics of variations of the total electron content (TEC) in the atmosphereare determined from data collected by GPS navigation satellites. An analysis of the observational
data showed that the spectrum of variations of the atmospheric and ionospheric parameters isindicative of acoustic-gravity waves (AGW) propagating from the lower atmosphere. The
observed manifestations of TEC disturbances caused by AGW propagating from the lower
atmosphere can be explained by the diurnal variation of the altitude of the ionosphere and thewaveguide propagation of infrasonic waves.
NUMERICAL MODELING OF NONLINEAR ACOUSTIC-GRAVITY WAVEPROPAGATION INTO THE UPPER ATMOSPHERE AT DIFFERENT LEVELSOF SOLAR ACTIVITY
Nikolai Gavrilov1, Sergei Kshevetskii2, Andrei Koval1
1
2Saint-Petersburg State University, Saint-Petersburg, Russia
Immanuel Kant Baltic Federal University, Kaliningrad, Russia

n.gavrilov@spbu.ru

According to present views, acoustic-gravity waves (AGWs) existing in the upper
atmosphere may be generated near the Earth’s surface due to different sources and propagate
upwards. An algorithm for three-dimensional numerical simulation of vertical propagation of
nonlinear AGWs from the Earth’s surface to the upper atmosphere was developed recently. The
algorithm of the solution of fluid dynamic equations uses finite-difference analogues of basic
conservation laws. This approach allows us to select physically correct generalized wave
solutions of the nonlinear equations. Horizontally moving horizontal sinusoidal structures of51

vertical velocity on the Earth’s surface serve as AGW sources in the model. Numericalsimulation was made in a region of the Earth atmosphere with dimensions up to several thousand
kilometers horizontally and 500 km vertically. Vertical profiles of the mean temperature, density,
molecular viscosity and thermal conductivity are specified from standard models of theatmosphere. Simulations are made for different amplitudes, horizontal wavelengths and speedsof wave sources at the lower boundary of the model. It is shown that after “switch on”
tropospheric source atmospheric waves very quickly (for several minutes) may propagate to highaltitudes (up to 100 km). When AGW amplitudes increase with height, waves may break downin the middle and upper atmosphere. Instability and dissipation of wave energy may lead toformations of wave accelerations of the mean winds and to creations of wave-induced jet flows
in the middle and upper atmosphere. Nonlinear interactions may lead to instabilities of the initialwave and to the creation of smaller-scale structures. These smaller inhomogeneities may increase
temperature and wind gradients and enhance the wave energy dissipation. Simulations withbackground wind and temperature profiles corresponding to small and high levels of solar activity
show that AGWs characteristics in the middle and upper atmosphere may change with changes insolar activity. This may alter heating and acceleration of the different layers of the atmosphere andchange conditions of dynamical coupling between the lower and upper atmosphere.
QUASI-BIENNIAL VARIATIONS IN IONOSPHERIC TIDAL/SPW AMPLITUDES:OBSERVATIONS AND MODELING
Loren Cheewei Chang1, Yan-Yi Sun2, Jack Chieh Wang1, Shih-Han Chien1,
Rung Tsai-Lin1, Jia Yue3
1

National Central University, Taiwan, Province of China
Kyushu University, Japan3
Hampton University, United States
2loren@ncu.edu.tw

In this study, we examine the coherent spatial and temporal modes dominating thevariation of selected ionospheric tidal and stationary planetary wave signatures from 2007–2013
FORMOSAT-3/COSMIC total electron content observations using Multi-dimensional Ensemble
Empirical Mode Decomposition (MEEMD) from the Hilbert-Huang Transform. We examine theDW1, SW2, DE3, and SPW4 components, which are driven by a variety of in-situ and vertical
coupling sources. The intrinsic mode functions (IMFs) resolved by MEEMD analysis allows forthe isolation of the dominant modes of variability for prominent ionospheric tidal / SPW
signatures in a manner not previously used, allowing the effects of specific drivers to be
examined individually. The time scales of the individual IMFs isolated for all tidal/SPW
signatures correspond to a semiannual variation at EIA latitudes maximizing at the equinoxes, aswell as annual oscillations at the EIA crests and troughs. All tidal / SPW signatures show one
IMF isolating an ionospheric quasi-biennial oscillation (QBO) in the equatorial latitudes
maximizing around January of odd numbered years. This TEC QBO variation is in phase with asimilar QBO variation isolated in both the GUVI zonal mean column O/N2 density ratio as wellas the F10.7 solar radio flux index around solar maximum, while showing temporal variation
more similar to that of GUVI O/N2 during the time around the 2008/2009 extended solar
minimum. These results point to both quasi-biennial variations in solar irradiance as well as
thermosphere / ionosphere composition as a generation mechanism for the ionospheric QBO. We
also present results from numerical experiments using the Thermosphere IonosphereElectrodynamics General Circulation Model (TIE-GCM) to quantify the sensitivity of thethermosphere and ionosphere to quasi-biennial oscillations in modulated atmospheric tides aswell as that present in F10.7. Our results are some of the first numerical experiments examining
the generation mechanisms behind the ionospheric QBO from both above and below.
52

ESTIMATING EQUATORIAL DAYTIME VERTICAL E×B DRIFT VELOCITIESFROM MAGNETIC FIELD VARIATIONS
Kassamba Abdel Aziz Diaby
Felix Houphouet Boigny University, Côte d’Ivoire
diabyaziz@yahoo.fr

Accurate measurement and prediction of the vertical plasma drift is important for the studyof many physical processes in the low-latitude ionosphere. Equatorial E×B drift velocities are
significant input parameters that go into many ionospheric models, because they help describe
vertical plasma motions near the magnetic equator. A previous work done by Anderson et al.
(2004) has demonstrated the ability to derive Peruvian longitude sector, daytime vertical E×B
drifts from ground-based magnetometer data and have derived the ΔH versus E×B relationships.
The present research extends the same method to the West African longitude sector. We use
magnetic field data of Conakry, Guinea (–0.46°, 60.37°) and Abidjan, Cote d’Ivoire (–6°,65.82°) from the African Meridian B-field Education and Research (AMBER) network. On thebasis of data availability, 9 magnetically quiet days have been analyzed and showed that the
Peruvian ΔH versus E×B relationships is applicable to the West African longitude sector.

A MATHEMATICAL MODEL OF QUASI-STATIONARY ELECTRIC FIELDPENETRATION FROM GROUND TO THE IONOSPHERE
Valery Denisenko
Institute of Computational Modelling SB RAS, Krasnoyarsk, Russia
denisen@icm.krasn.ru

A quasi-stationary model of electric fields and currents in the conductor that includes the
Earth’s atmosphere and ionosphere is created. We use an empirical model of scalar conductivity
in the main part of the atmosphere up to the height of 50 km and a model of tensor conductivity,
based on the empirical models IRI, MSISE, IGRF above 90 km with smooth interpolation
between these layers. The steady state electro-conductivity problem is numerically solved. We
set the input parameters which look typical for moderate earthquakes like a vertical electric fieldof about 100 V/m near ground with typical horizontal scale of a few hundred km. The result
electric field in the ionosphere in such a case does not exceed 0.001 mV/m in frame of our model.
This means that the penetration of a large scale electric field from ground into the ionospherecannot be a physical process which creates ionospheric precursors of earthquakes which areobserved in range of a few mV/m. This conclusion has been previously published, but it
contradicts to the mathematical models by other authors. Here we analyze these models andshow that their authors used inappropriate assumptions or simplifications which significantly
distort the results. At the same time one of the new models confirms our conclusion.

53

SINGULAR VALUE DECOMPOSITION BASED ANALYSIS SOLAR ACTIVITY
IN THE IONOSPHERE USING TOTAL ELECTRON CONTENT MAPS
Cenk Toker, Feza Arikan
Hacettepe University, Ankara, Turkey
arikan@hacettepe.edu.tr

Singular value decomposition (SVD) is a well-established technique in linear algebra, and
it is widely used to analyse signals in various fields of signal processing. Total electron content(TEC) is one of the most important observables of ionosphere and the TEC variability is directly
related to the structural changes in the ionosphere. Solar activity is the driving force ofionosphere whose spatio-temporal trend is aligned with 11-year, annual, seasonal, monthly anddiurnal cycles. One of the most commonly methods to estimate TEC is the use of dual-frequency
GPS receivers. For spatial sparsity, GPS-TEC values obtained from various receivers in a certain
area are interpolated to obtain a spatial distribution of TEC which is called as a TEC map. In thisstudy, SVD method is applied to TEC maps for analysis of solar activity in the ionosphere. Morespecifically, we investigate the behavior of singular values of the TEC map for different
ionospheric conditions. If the TEC map of a certain region is discretised in space and organized
as a matrix, SVD can be applied to provide singular values and corresponding singular vectors
representing the energy content of the TEC map. The first singular value contains most of theenergy present in the image, and it provides information about large scale — low frequency(trend-like) variations in the TEC map. The second and third singular values are generally twoorders of magnitude smaller compared to the first one, and these singular values represent thesecondary spatio-temporal variabilities that are related to the factors other than solar activity
such as gravitational, geomagnetic or seismic in nature. The TEC map can be reconstructedusing the first three or four singular vectors as an image. In this study, singular values of regional
TEC maps from Central Europe are investigated for quiet, positively disturbed and negatively
disturbed ionospheric conditions. It has been observed that the first singular value represent thestrong trend structure of ionosphere related directly to the solar activity. The first singular modeis enough to reconstruct the TEC map with an error less than 1 %. The second, third and fourth
singular values are more related to geomagnetic and seismic disturbances and the values of theselower order modes increase related to the intensity of the disturbances in the ionosphere.
SQ CHANGES RELATED TO EARTH’S MAGNETIC FIELD SECULAR VARIATIONSAND SOLAR ACTIVITY EFFECTS
Blas de Haro Barbas, Bruno Zossi, Ana Elias
Instituto de Física Universidad Nacional de Tucuman, Argentina
blasdeharo2000@yahoo.com.ar

Variations in the solar quiet geomagnetic field (Sq) are mainly caused by the ionosphericcurrent systems which flow in the E-region driven by electric fields generated by theatmospheric dynamo. The main variables in Sq are ionospheric conductivities, the dynamo
electric field, the solar diurnal tide and the E-region electron concentration. In turn, solar EUV
irradiance and Earth’s magnetic field are among the variables involved in ionosphericconductivity. Both present changes, and so does their contribution to ionospheric conductivity
and so, to Sq. Considering the theoretical equations of Hall and Pedersen conductivity, the effectof solar activity and Earth magnetic field variations are analyzed comparatively. An
experimental analysis is also carried out using Sq variation of the horizontal intensity, H, ofmagnetic observatories at low and mid-latitudes.
54

IONOSPHERIC CONDUCTING LAYER HEIGHT CHANGESDUE TO GEOMAGNETIC SECULAR VARIATIONS AND SOLAR ACTIVITY LEVEL
Blas de Haro Barbas, Bruno Zossi, Ana Elias
Instituto de Física Universidad Nacional de Tucuman, Argentina
blasdeharo2000@yahoo.com.ar

Ionospheric conductivity, a critical element in magnetosphere-ionosphere-thermosphere
coupling and ionospheric electrodynamics in general, responds to several forcings. Among them, theEarth’s magnetic field, which determines not only the conductivity magnitude but also the height ofthe conducting layer. This field that varies greatly in geological timescales, can be approximated by amagnetic dipole that accounts for ~80 % of the magnetic field of the Earth’s surface, plus multipolar
components making up the remaining ~20 %. We analyze in this work the effects over the
conducting layer height of the secular variations of the Earth’s magnetic field considering that duringa polarity transition the field magnitude diminishes to about 10 % of its normal value at the expenseof decreasing the dipolar component and becoming mostly multipolar in nature. In general, a field
decrease lifts the ionospheric conducting layer to regions where the electron density is higher,
eventually reaching the F layer. Height changes are compared to variations induced by solar activity
level through its effect on the scale height and neutral density.
IONOSPHERIC DISTURBANCES AFTER THE MAIN PHASEOF GEOMAGNETIC STORM
Maxim V. Klimenko1,2, Vladimir Klimenko1, Konstantin Ratovsky3, Alexei Dmitriev4,5,Alla Suvorova4,5, Irina Zakharenkova1
1

West Department of Pushkov IZMIRAN, RAS, Kaliningrad, Russia
Immanuel Kant Baltic Federal University, Kaliningrad, Russia
3
Institute of Solar-Terrestrial Physics, SB RAS, Irkutsk, Russia
4
Institute of Space Science, National Central University, Jhongli, Taiwan
5
Skobeltsyn Institute of Nuclear Physics, Lomonosov Moscow State University, Moscow, Russia
2

maksim.klimenko@mail.ru

We present an overview of the ionospheric effects of geomagnetic storms occurred on
September 26–30, 2011 and March 17–23, 2015 during recovery storm phases. The results wereobtained from both the satellite and ground-based observations, and from the computer
simulation using the Global Self-consistent Model of the Thermosphere, Ionosphere, andProtonosphere (GSM TIP). The simultaneous formation of positive disturbances in foF2 andnegative disturbances in TEC at low latitudes during the storm’s recovery phase are explained by
the plasma tube diffusional depletion, which is the main formation mechanism of the negative
perturbations in TEC at this storm period. We have found that in general, the GSM TIP modelgave a reasonable prediction of both positive and negative ionospheric storms. We are facing thegreatest difficulties for the St. Patrick’s Day storms. Namely, a strong positive storm at low
latitudes above the Pacific and SAA region on the recovery phase could not be predicted by themodel. Though the positive storm could be explained by the ionization effect of energetic
electron precipitation enhancements. During the storm recovery phase in the low, middle andsubauroral latitudes the model results show an increase in the n(O)/n(N2) ratio and a decrease in
the n(N2) that results in the daytime positive effects in the NmF2. We checked how thisconclusion can be generalized to other geomagnetic storms. For testing we used the 2003–2016
Irkutsk ionosonde (52.3° N, 104.3° E) data set.
55

SEASONAL ANOMALIES AND VARIATIONS IN EQUINOXAND SOLSTICE PERIODS IN IONOSPHERE OVER TURKEY
Secil Karatay1, Ali Cinar1, Feza Arikan2
1
2

Kastamonu University, Kastamonu, Turkey
Hacettepe University, Ankara, Turkey

skaratay@kastamonu.edu.tr

A region of the upper atmosphere of the Earth is called as the ionosphere that extends from 50
km to 1000 km. Ionospheric electron density is the major point to investigate the spatial and temporalvariations in the ionosphere. Total Electron Content (TEC) is the integral of the electron density
along the ray-path between the transmitting satellite and the receiver. Global Positioning System(GPS) is tool for monitoring the electron distribution within the ionosphere. One of the most usedsolar indices is the Sun Spot Number defined to measure the number of sun spots and groups of sun
spots on the surface of the sun that appear visibly as dark spots compared to surrounding regions.
SSN decreases and increases over a period of approximately 11 years. This study is focused on theanalysis of the variations of ionosphere over Turkey during equinox and solstice periods using
IONOLAB-TEC estimates obtained by GPS. Bite-out phenomenon is examined for discovering its
possible effects. It is observed that bite-out predominantly occurs in winter for minimum Sun Spots
Numbers (SSN) in the middle zones of Turkey. The middle zones of Turkey are also significantly
affected from the winter anomaly. TEC values and ionospheric variations at solstice periods are
greater than those at equinox periods. This study is supported by TUBITAK EEEAG grant 114E541
and joint TUBITAK EEEAG 114E092 and AS CR 14/001.
COMPARISON OF NMF2 SOLAR ACTIVITY DEPENDENCE OVER KALININGRAD
AND IRKUTSK — EMPIRICAL MODEL’S RESULTS
Nikolay Chirik1, Alexander Markov2, Maxim V. Klimenko1,2, Konstantin Ratovsky3,
Alexander Karpachev4, Vladimir Klimenko1, Lubov Pustovalova4, Nina Korenkova1
1

West Department of Pushkov Institute of Terrestrial Magnetism, Ionosphere and Radio Wave
Propagation RAS, Kaliningrad, Russia
2
Immanuel Kant Baltic Federal University, Kaliningrad, Russia
2
Immanuel Kant Baltic Federal University, Kaliningrad, Russia
3
Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
4
Pushkov Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation RAS,
Moscow, Russia
maksim.klimenko@mail.ru

In this report we have analyzed the solar activity dependence of the NmF2 diurnal
variations for different seasons over two mid-latitude stations Irkutsk and Kaliningrad. In orderto estimate the solar activity dependence of NmF2 diurnal variation we used the empirical models
based on the statistical analysis of ground based ionosonde data, satellite and radio occultation
measurements. For the local empirical model development, we used the database of NmF2
observation data from the Irkutsk and Kaliningrad ionosondes. These data were obtained fromthe manually scaled ionograms using interactive ionogram scaling software, SAO Explorer in thecase of the Irkutsk ionosonde and PARUS software in the case of the Kaliningrad ionosonde.
The geographic latitudes of both stations are very similar. We obtained the 27-daily median of
NmF2 values for diurnal variations over two these stations for different months. We analyzed andcompared the coefficients and mean squared errors of linear and dual linear regression for both
stations. Also, we used the radio occultation NmF2 values, IRI and MIT modeling in order tocompare local empirical model results with global empirical models of different kinds.
56

UNUSUAL EVOLUTION OF PLASMA BUBBLES INTO NON-CONJUGATEFEATURES DURING 17 MARCH 2015 STORM
Lakshmi Narayanan Viswanathan1, Sukanta Sau2, Subramanian Gurubaran3,
Rupesh Ghodpage4, P.T. Patil4
1

National Atmospheric Research Laboratory, Gadanki, India
Equatorial Geophysical Research Laboratory, Indian Institute of Geomagnetism, Tirunelveli, India
3
Indian Institute of Geomagnetism, Navi Mumbai, India
4
MF radar Facility, Indian Institute of Geomagnetism, Shivaji University Campus, Kolhapur, India
2

narayananvlwins@gmail.com

We study the equatorial plasma bubbles occurred over the Indian region during the 17 March
2015 geomagnetic storm using OI 630 nm airglow imaging from two locations Kolhapur (16.7° N,
74.3° E, 11.5° N dip latitude) and Tirunelveli (8.7° N, 77.8° E, 1.6° N dip latitude). Since
airglow imaging technique covers large area, we could observe the region between 5° S and 18° N
dip latitudes. Though several works have already been reported about the effects of the 17 March
2015 storm, we present results that are unique and not identified earlier. The plasma bubble
zonal drifts on this night changed from east to west. Interestingly, the portions of the bubbles
mapped to higher latitudes were seen to reverse their zonal drift before the portions closer to thedip equator reversed. Simultaneously the westward tilt of the bubbles increased considerably.
Subsequently, the plasma bubbles were seen to evolve into non-conjugate features between thehemispheres within 4° of the dip equator. To our knowledge no earlier report has identified nonconjugate plasma bubbles. Also significant differences are noticed in the drifts between theadjacent bubbles for a short duration. These results are discussed in the light of current
understanding of the low latitude electrodynamics.

THE EARTH’S ATMOSPHERE IONIZATION RATE CALCULATION WITH
THE RUSCOSMICS SOFTWARE PACKAGE
Eugeny Maurchev
Polar Geophysical Institute, Apatity, Russia
maurchev1987@gmail.com

To solve some problems, e.g. the equivalent dose evaluation at altitudes of 10 km, it isneeded to know the ionization rate of the Earth’s atmosphere matter by cosmic rays (CR) in theabsence of disturbances and during the solar flares (The SCR events).In this work the passage ofcosmic-ray protons through the Earth’s atmosphere by numerical Monte Carlo methods arecalculated. The main characteristics of the CR secondary fluxes and the ionization profiles
depending on a primary particle energy and a geomagnetic cutoff rigidity are presented. The
results allow to quantify the equivalent dose for the different heights of the Earth’s atmosphere.

57

SOLAR SIGNATURES WITHIN ATMOSPHERIC
AND IONOSPHERIC PARAMETERS
Petra Koucka Knizova1, Katya Georgieva2, Zbysek Mosna1, Boian Kirov2, Daniel Kouba1
12Institute of Atmospheric Physics of Czech Academy of Sciences, Prague, Czech Republic
Space Research and Technology Institute of Bulgarian Academy of Sciences, Sofia, Bulgaria

pkn@ufa.cas.cz

We have analyzed time series of solar data together with the atmospheric and ionosphericmeasurements for last four solar cycles according to their availability. Within data of 1-day
sampling rate, we have searched for common spectral domains. As a convenient mathematical
tool we used Continuous Wavelet Transform (CWT) that is favorable for detection of wave-likeoscillations with limited duration and variable period. Then we looked for common oscillation
domains in the datasets using Wavelet Transform Coherence (WTC), which is a measure of theintensity of the covariance of the two series in time-period space with stable phase difference.
Despite wide oscillation ranges detected by mean of CWT we found only limited domains bymean of WTC, particularly significant high power domains (with stable phase difference) for
periods 1 month, 2 months, 6 months, 1 year and 2 years between pairs of solar data, andatmospheric or ionospheric data. The detected domains vary during particular solar cycle andfrom cycle to the following one. These results indicate the changing solar forcing of theatmosphere and/or its sensitivity with time.

SOLAR CYCLE IN UV AND ITS RESPONSE IN D-REGION (3D SIMULATIONS)
Alexei Krivolutsky, Lidiya Cherepanova
Central Aerological Observatory, Dolgoprudny, Moscow, Russia
krivolutsky@mail.ru

3D photochemical simulations with CHARM-I (Chemical Atmospheric Research Modelwith Ions [Krivolutsky et al., 2015]) to study changes in D-region induced by solar UVvariations during 2003–2009. This interval belongs to 23rd solar cycle with a deep minima
between 2007 of global electron concentration fields between 2009 and 2003 (from minima to
maxima) was calculated. The results of simulations showed that corresponding changes ofelectron density for day time conditions equaled about 30 % with minus above 70 km. At thesame time a weak increase of [e] was found in zonal mean fields around 60 km.

58INFRA-RED TEMPERATURE MAPPING STUDIESOF MESOSPHERIC GRAVITY WAVES
Michael John Taylor1, Pierre-Dominique Pautet1, Yucheng Zhao1, Neal Criddle1,
Pattilyn McLaughlin1, W.R. Pedlenton Jr.1, David Fritts2, Gunter Stober3,
Franz-Josef Lübken3, Bernd Kaifler4, Markus Rapp4, Steve Smith5, Ben Liley6
1

Utah State University, Logan, United States
GATS Incorporated, Boulder, United States
3
Leibniz-Institute of Atmospheric Physics (IAP), Kühlungsborn, Germany
4German Aerospace Center/DLR, Institute of Atmospheric Physics, Oberpfaffenhofen, Germany
5Center for Space Physics, Boston University, United States
6
NIWA, Lauder Observatory, Central Otago, New Zealand2

mike.taylor@usu.edu

The Advanced Mesospheric Temperature Mapper (AMTM) is a wide-field (120°) highperformance digital imaging system developed at Utah State University. The AMTM is capableof precision measurements of the OH(3.1) band intensity and rotational temperature (~1–2 K in
< 30 s) important for quantifying the effects of a broad-spectrum of gravity waves at the ~87 km
level, with periods ranging from several minutes to many hours. This presentation highlights
measurement capabilities, and recent results from several focused campaigns employing coordinatedlidar, radar and AMTM measurements to quantify the properties and momentum fluxes ofmesospheric gravity waves, including orographic waves generated by the interaction of strong winds
with prominent mountain ranges. Mountain waves are identified by their quasi-stationary appearance,
and until recently, observations of their penetration into the mesosphere and characteristic
signatures have been very sparse. Selected studies include gravity wave propagation, dissipationand temperature signatures in the high Arctic and over Antarctica, and mountain wave breaking
at mesopause heights during the DEEPWAVE program (June–July 2014) where two AMTM’swere operated from New Zealand in the vicinity of an intense gravity wave “hot spot”.
EQUATORIAL IONOSPHERIC VARIATIONS CAUSED BY
THE DIFFERENT LARGE SCALE SOLAR WIND STRUCTURES
Lilia Biktash
Pushkov Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation RAS,
Moscow, Russia
lilia_biktash@mail.ru

We examined equatorial ionospheric variations during geomagnetic storms associated withlarge scale solar wind structures. Yohkoh, SOHO and Ulysses missions proved that in general,the mass emissions from the Sun as interplanetary coronal mass ejections (ICMEs), corotatinginteraction regions (CIRs), and heliospheric current sheet (HCS) are responsible for generationof different types of geomagnetic storms. Intensive ionospheric currents during thesegeomagnetic storms change the quiet ionosphere and short-term variations of the ionosphericcharacteristics are observed. Under these conditions the critical frequency foF2, virtual height h’F,
drift velocities and others ionospheric characteristics are mainly defined by the the state of thesolar wind flowing around the Earths magnetosphere. We show that these variations are defined
to a significant degree by the direction of the Bz component of the interplanetary magnetic field
but duration and intensity of these variations determined by the origin of the solar wind streams(CMIs, CIRs or HCS). The ionospheric heights and foF2 variations at the equator during thenorthward IMF Bz and the southward IMF Bz (the main phase of the magnetic storm) are very59

distinguished. Distinction between quiet and disturbance periods in the heights can reach up
to100 km and more. The critical frequency foF2 is markedly lower during the southward IMF Bz.
We show also that intensity of the equatorial ionospheric variations is different for the same solar
wind conditions and depends on solar activity phases.
LONG TERM METEOR RADAR OBSERVATIONS OF GRAVITY WAVE ACTIVITY
IN THE MESOSPHERIC LOWER THERMOSPHERIC REGIONOVER A LOW LATITUDE STATIONMaria Antonita Thithonis
Indian Space Research Organisation, Bangalore, India
mariaspl@gmail.com

Gravity waves play a profound role in the vertical coupling of the different regions of the
Earth’s atmosphere. Divergence/convergence of the energy and momentum fluxes carried by thegravity waves accelerate/ decelerate the mean flow which in turn partly responsible for the
maintenance of QBO and SAO in the stratospheric and mesospheric region, which are thecharacteristic features of the equatorial middle atmosphere. To quantify the role of short period
gravity waves in controlling the dynamics of the MLT region, more than ten years of continuous
meteor radar observations during June 2004 – Dec 2013 are extensively used. The gravity wave
activity in the Mesosphere Lower Thermosphere (MLT) region is estimated over Trivandrum(8.5° N, 78° E), a low-latitude station in India during aforementioned period. The seasonal, interannual variation and solar cycle variability of the wave activity is also examined. The results will
be discussed in detail in the conference.
SOLAR AND METEOROLOGICAL CONTROL OF THE HIGH-FRIEQUENCYTOTAL ELECTRON CONTENT VARIABILITY
Anna Yasyukevich, Marina Chernigovskaya,
Anna Mylnikova, Boris Shpynev
Institute of Solar-Terrestrial Physics of SB RAS, Irkutsk, Russia
annpol@iszf.irk.ru

We study seasonal and helio-geomagnetic activity pattern of total electron content (TEC)
variability over Siberia region during the 2002–2015 period. The considered years cover interval
between the 23th and the 24th solar activity cycle peaks. For the analysis of TEC behavior wehave used data from phase dual frequency GPS/GLONASS receivers located in mid-latitude(Irkutsk, 52° N, 104° E; 42° N Glat, 177° E Glon), subauroral (Yakutsk, 62° N, 130° E; 52° N Glat,
196° E Glon) and high-latitude (Norilsk, 69° N, 88° E; 60° N Glat, 166° E Glon; Tixi, 72° N, 129° E;
66° N Glat, 198° E Glon) regions and have calculated an index of intensity of TEC variation(vrTEC) with periods of up to 4 hours. The index is a relative standard TEC deviation from thedaily average values in daytime. Obtained vrTEC coefficient reflects ionospheric variability
associated with internal gravity waves (IGWs) propagation. It is revealed that TEC variability
level depends on the solar activity during winter seasons. Maximum winter vrTEC values reduceof up to 40 % at the solar activity descending stage. The effect is more pronounced at highlatitudes. Surprisingly, the TEC variability level does not change with solar activity in summer
months. It has been shown for all the stations considered that there are significant changes in the60

TEC variation coefficient with seasons. The largest values is observed in winter and the smallest
ones in summer. The summer-winter vrTEC difference is more noticeable for high-latitude
stations (Norilsk and Tiksi) and reaches up to 6 times. Such seasonal vrTEC variations are
regularly observed from year to year. The winter enhancement of the high-frequency part of the
TEC variability is assumed to be induced by medium-scale wave-like motions in the stratosphereand mesosphere. The sources of these motions are instabilities in the spatially non-uniform, highvelocity jet stream on the boundary of circumpolar vortex (CPV) forming in winter hemisphere.
Traveling upward, the medium-scale waves cause changes in the lower thermosphere andionosphere structure and dynamics and manifest themselves as traveling ionospheric disturbances.
This study is supported by RF President Grant of Public Support for RF Leading Scientific Schools(НШ-2942.2014.5) and by the RFBR projects No. 16-35-60018 and 15-05-05227.

SOURCES OF THE IONOSPHERIC VARIABILITY OVER EUROPE IN WINTER
TIME FROM THE IONOSONDE AND GPS/GLONASS DATA
Boris Shpynev1, Marina Chernigovskaya1, Anna Yasyukevich1, Anna Mylnikova1,
Petra Koucká Knížová2, Daniel Kouba2, Jens Mielich3,
Alexander Kozlovsky4, Bruno Zolesi5

1Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
Institute of Atmospheric Physics CAS, Prague, Czech Republic
3
Leibniz Institute for Atmospheric Physics, Kühlungsborn, Germany
4
Sodankylä Geophysical Observatory, Sodankylä, Finland
5
The Istituto Nazionale di Geofisica e Vulcanologia, Rome, Italy2shpynev@iszf.irk.ru

The latitudinal dependence of ionospheric variability on the configuration and parametersof high-speed jet streams associated with the winter circumpolar vortex at the stratosphere/lower
mesosphere heights are studied. We conducted a joint analysis of the variations of theionospheric F2-layer electron density peak and total electron content (TEC) of the ionosphere
over the mid- and high-latitude regions of Europe in the winter months (November to February)
over 2008–2010 under low solar and geomagnetic activity conditions. The ionosphereparameters were obtained from measurements made at the meridional chain of European verticalsounding ionosondes Rome (41.9° N, 12.5° E), Pruhonice (50.0° N, 14.6° E), Juliusruh (54.6° N,
13.4° E), Sodankylä (67.3° N, 26.6° E). The measurements on a network of the phase dualfrequency GPS/GLONASS receivers located in the range of 40–70° N and 10–30° E were used
to obtain TEC. The calculation of the vertical total electron content from the initial series was
based on the developed absolute TEC model taking into account differential code biases. To
study the dynamics of the winter circumpolar vortex in the Northern Hemisphere, we use thedata from the ECMWF ERA-Interim Reanalysis. The analysis showed the significant increase inwave-like activity in the stratosphere/lower mesosphere during winter seasons for all analyzed
years. Variations of ionospheric parameters observed at different latitudes depend on the station
positions relative to the jet stream circulation zone.

61THE CHELYABINSK METEORITE EFFECTS IN IONOSPHERE
ACCORDING TO THE GPS NETWORK DATA
Natalia Perevalova1, Nikolay Shestakov2, Sergey Voeykov1
1
2

Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
Far Eastern Federal University, Institute of Applied Mathematics FEB RAS, Vladivostok, Russia

pereval@iszf.irk.ru

We present the results of studying characteristics of ionospheric effects of the Chelyabinsk
meteorite. The results are based on the unique data from several GPS networks located in thevicinity of the final part of the meteorite fall trajectory. GPS receivers detected two kinds oftraveling ionospheric disturbances (TIDs) in total electron content (TEC) variations triggered by
the meteorite fall and explosion. 6–14 min after the meteorite explosion, a TID with a cone-shaped
wavefront was observed at the 80–100 km distance from the airburst location. The averaged TID
propagation velocity was 661 m/s. We associated this TID with shock-acoustic waves (SAW). 14
min after the meteorite explosion, behavior of the TEC disturbances complied with the annular
wavefront propagating with the averaged velocity of 337 m/s from the center which was locatedapproximately 37 km northwestward of the airburst. The annular front was formed approximately
200 km away from the meteorite explosion location. The annular TID velocity damping with timeand distance from the airburst was estimated using the GPS interferometric technique. This TID
was interpreted as gravitational mode of internal atmospheric waves.
The data from the global GPS network were provided by Scripps Orbit and Permanent
Array Centre (SOPAC, http://sopac.ucsd.edu). The data from the Russian GPS network operated
by the NAVGEOKOM company were available at http://www.navgeocom.ru. Raw TEC data
and auxiliary information from GPS stations in the Chelyabinsk region were kindly provided by
LLC GEOSalyut (Moscow) and LLC Poleos (Chelyabinsk, contact with shestakov.nv@dvfu.ru).
Raw TEC data and supporting information from GPS stations in the Chelyabinsk region were
provided by LLC GEOSalyut (Moscow) and LLC Poleos (Chelyabinsk, contact withshestakov.nv@dvfu.ru). Raw TEC data and supporting information from the Kazan GPS
network were provided by Federal Kazan University (KFU) and RPC Geopoligon KFU (Kazan,
contact with shestakov.nv@dvfu.r). We are deeply indebted to all companies and agencies andpersonally to S. Parshin provided us with access to GPS data. This work was supported by the
Presidium of the Russian Academy of Sciences (program No. 15, project No. 0344-2015-0019
Study of the Lithosphere–Atmosphere–Ionosphere System under Extreme Conditions), RF
President Grant of Public Support for RF Leading Scientific Schools (НШ-6894.2016.5), and
RFBR grant No. 17-55-53110 GFEN_a.
EXPERIMENTAL STUDY OF IGW-WIND INTERACTION USING THE COMBINEDIRKUTSK INCOHERENT SCATTER RADAR AND IONOSONDE DATA
Andrey Medvedev, Konstantin Ratovsky, Maxim Tolstikov, Sergey Alsatkin
Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
maxim@iszf.irk.ru

This paper studies the interaction of internal gravity waves (IGW) with neutral wind using
the statistics of traveling ionospheric disturbances (TID) from the Radio Physical Complex of theInstitute of Solar-Terrestrial Physics. The simultaneous measurements of Irkutsk incoherent
radar and ionosonde DSP-4 allows us to obtain representative statistic of TIDs parameters,
including full velocity vector. Measurement of TID full velocity vector allow us to separate IGW
62

induced TIDs from TIDs of other nature. Selecting of IGWs induced TIDs by estimating of
neutral wind velocity projection on TID propagation direction, show that ~60 % TID induced by
IGW. TIDs distribution on time and IGWs distribution on time have significant difference.
Number of nighttime TIDs, especially in winter season, is much bigger then daytime TIDs, but
for IGW induced TIDs distributions are more evenly. Assuming fulfillment of Hines dispersion
equation, average diurnal variation of meridional and zonal wind for winter, spring and summer
seasons were obtained. There are very few direct measurements of meridional and especiallyzonal neutral winds at ionospheric heights. Therefore, indirect estimations of neutral winds basedon measurements of TID three-dimensional velocity vector, can be very useful to neutral windmodel improvement. Shown that the main cause of the observed anisotropy of TIDs characteristics
associated with filtration IGWs by neutral wind. IGWs, propagating against the neutral wind at
observations heights, increase amplitudes, and azimuths, co-directional with a strong neutral wind(over 50 m/s) on any of the heights through which IGWs passed before reaching observation height,
were prohibited. Most of TIDs (83 %) have a downward phase velocity (negative elevation angle),which corresponds to IGW propagating from the source located under the region considered. Positive
elevation angles, can be divided into two ranges: 0–45° (reflected TIDs ~9 %) and 45–90° (TIDsfrom sources above observation area ~8 %). Peculiarities of TIDs azimuths distributions for this three
IGW types were also well explained by the neutral wind. The present work was done under supportof the Russian fund of basic research (grant No. 15-05-02313).
IMPACT OF STRATOSPHERIC WARMINGS ON THE MLT COMPOSITION
AND TEMPERATURE FROM SPECTROMETRIC OBSERVATIONS OF OH (6-2)
AIRGLOW AT MID LATITUDES
Irina Medvedeva1, Anatoly Semenov2
1
2

Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
Obukhov Institute of Atmospheric Physics RAS, Moscow, Russia

ivmed@iszf.irk.ru

We present the results of studying the atmospheric composition and temperature
disturbances at the mesosphere and low thermosphere (MLT) associated with sudden
stratospheric warmings (SSWs) in 2010–2017. Several events related to different types ofstratospheric warming (major, minor, final) were selected for the analysis. We analyzed the dataon the OH emission intensity and rotational temperature derived from spectrometricmeasurements of the hydroxyl emission (834.0 nm, band (6-2)) at the Geophysical Observatoryof the Institute of Solar-Terrestrial Physics (51.8° N, 103.1° E) and at the Zvenigorod station of
the Obukhov Institute of Atmospheric Physics (55.7° N, 36.8° E). The OH emission maximum isat the mesopause region height (~87 km). The OH molecule rotational temperature is determinedwith a 1–2 K accuracy and corresponds to the atmosphere temperature at the radiation height.
The emission intensity provides information on the dynamics of photochemical processes andrecombination of atomic oxygen at the emission layer heights. The data on OH (6-2) rotationaltemperature and intensity were used to calculate variations in the atomic oxygen density in the
MLT during the analyzed stratospheric warmings. In the calculations, we used thephotochemical model of OH emission and the NRLMSISE-00 atmospheric model. It is shown,that significant SSW events can cause an increase in the intensity of OH emission (6-2) and in
the atomic oxygen density at the height of the OH layer by more than 2.5 times. The revealed
effect can be caused by the SSW-related increase in vertical transfer of the atmosphericcomponents. This study was done with a support from the Russian Foundation for Basic
Research, Grant No. 17-05-00192-a, and RF President Grant of Public Support for RF Leading
Scientific Schools (НШ-6894.2016.5). Experimental data recorded by the Angara MultiaccessCenter facilities of ISTP SB RAS were used.
63

STATISTICS OF IONOSPHERIC DISTURBANCES DURING SUDDENSTRATOSPHERIC WARMINGS OVER EASTERN SIBERIA
Konstantin Ratovsky, Irina Medvedeva
Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
ratovsky@iszf.irk.ru

We study statistics of ionospheric disturbances during sudden stratospheric warmings(SSWs)) over Eastern Siberia. The statistics is based on the 2003–2016 dataset of F2 peakelectron density (NmF2) from Irkutsk DPS-4 Digisonde (52.3° N, 104.3° E). Atmospherictemperature and dynamics during SSWs were analyzed from Aura MLS v3.3 satellite data and
MERRA reanalysis. As onsets of SSW events we chose the days of reversal in longitudinallyaveraged zonal wind at 60° N and 10 hPa (in cases of major SSWs) or days of the largest
temperature at 10 hPa (in cases of minor SSWs). Further we analyze day-to-day behaviors of
NmF2 disturbances over the 20-day intervals after the SSW onsets. The NmF2 disturbances are
the percentage differences between the observed NmF2 (NmF2obs) and the 27-day sliding medianvalue (NmF2med): dNmF2(%)=(NmF2obs–NmF2med)/NmF2 med 100 %. In order to reveal positive
and negative ionospheric effects of the SSW events we consider the day-to-day variations in thedaytime and nighttime averaged NmF2 disturbances. For studying intensification of wave activity
during the SSW events we analyze the intensity of the NmF2 disturbances in different period
ranges: the internal gravity wave period range (periods T<8 hrs) and the tidal range (8 hrs ≤ T ≤24 hrs). The intensities of the NmF2 disturbances are the root mean square values of disturbances
calculated for the given day. The comparison of the obtained disturbance intensities with thebackground level of the ionospheric variability allows us to make conclusion about the SSW
effects on the intensification of ionospheric wave activity. The 2003–2016 dataset of NmF2
allows us to analyze the ionospheric responses to the 7 minor and 7 major SSW events. The
work was supported by RF President Grant of Public Support for RF Leading Scientific Schools(НШ-6894.2016.5) and the Russian Foundation for Basic Research, Grant No. 17-05-00192-a.
Experimental data recorded by the Angara Multiaccess Center facilities of ISTP SB RAS were used.
COMPARISON OF THE LEVEL OF IONOSPHERE DISTURBANCEAT SEVERAL GNSS STATIONSOlga Timofeeva1, Natalia Perevalova2, Darya Katashevtseva1, Ilya Edemskiy2
1
2

Irkutsk State University, Irkutsk, Russia
Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia

olga.timofeeva.1994@yandex.ru

Using special WTEC index, we compared the level of ionosphere disturbance at three
GNSS stations: BADG (mid latitudes), TIXI and NRIL (high latitudes) in 2013. WTEC iscalculated from the total electron content (TEC) obtained by GNSS receiver. WTEC represents
continuous multi-day series of average TEC variation intensity for the selected range of periods.
We studied the TEC disturbances with periods of 10 min (middle-scale ionospheric disturbances)and 40 min (large-scale ionospheric disturbances). At the BADG station, the WTEC minimum
level is higher in summer than in winter. The WTEC daily variations are pronounced throughout
a year and have some features: from April to October, depression in manifestation of the WTEC
diurnal variations is observed for medium-scale disturbances, from June to September the same
is fair for large-scale disturbances; large amplitude of diurnal variations are typical for WTEC
variations from October to December. The WTEC behavior agrees well with the Dst and Kp
64

variations only during strong magnetic storms. At TIXI and NRIL stations, the WTEC minimum
level does not depend on the season. The WTEC diurnal variations are weakly pronounced andmore evident for medium-scale disturbances than for large-scale ones. The WTEC index
behavior accords well with the AE geomagnetic index variations; it is less consistent with Dst
and Kp indices behavior; only in severe planetary magnetic storms, the WTEC behavior agrees
with the Dst behavior. This work was supported by the Grant of the Russian ScientificFoundation (Project No. 14-37-00027).
BEHAVIOR OF IONOSPHERIC TOTAL ELECTRON CONTENT
IN THE HIGH LATITUDES ON 4–6 MAY 2013
Darya Katashevtseva1, Natalia Perevalova2, Olga Timofeeva1, †Elena Romanova2
1
2

Irkutsk State University, Irkutsk, Russia
Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia

dasyadk@gmail.com

We present the results of a study of the total electron content (TEC) spatial-temporal
distribution in the high-latitude ionosphere on 4–6 May, 2013. We used the data from highlatitude GPS stations being a part of the International GNSS Service (IGS) network: LOVJ
(Murmansk), NRIL (Norilsk), TIXI (Tiksi), BILB (Bilibino). For analysis we used only thosesatellites that were in the radio visibility zone of NRIL, LOVJ, TIXI, BILB within the 04:00–
10:00 UT time period. The analysis revealed that on May 5, 2013, on some GPS receiversatellite lines of sight, there were dramatic TEC deviations from the behavior typical for control
days on May 4 and 6. This indicates that there was an ionization trough (a low electron density
region) in the ionosphere at these latitudes. To determine the trough position, we plotted the
trajectories of the ionospheric points, where the TEC deviations were recorded. The ionization
trough was located within the 72–84 N latitudes and 0–200 E longitudes. We compared theexperimental results with the numerical simulation data. Using the ionosphere-plasma interaction
theoretical model, developed in ISTP SB RAS, global distributions of the thermal plasma
characteristics for 05:00 UT and 07:00 UT on May 5, 2013 were calculated. This model showedthat at high latitudes on the day side in the same range of latitudes and longitudes, a region of
reduced TEC values can form, which can be identified as a high latitude trough. This work was
supported by the Grant of the Russian Scientific Foundation (Project No. 14-37-00027).
BURSTS OF MAGNETOSPHERE CHARGED PARTICLE FLUXESAND VARIOUS TYPES OF GEOMSGNETIC PULSATIONS
AND ATMOSPHERE GLOWS DURING THE SUPERSTORMAT MIDDLE LATITUDES NEAR IRKUTSK
Yulia Klibanova1, Vladimir Mishin1, Battuulai Tsegmed2
1

Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
Research Center of Astronomy and Geophysics of Mongolian Academy of Sciences, Ulaanbaatar,
Mongolia
2

malozemova81@mail.ru

We study variations of broadband geomagnetic pulsations and charged particle fluxes in
the magnetosphere during the atmosphere glows at midlatitudes during the two superstorms.
Geomagnetic and optical data of the ground-based observatories of the ISTP SB RAS are used,65

as well as satellite data of the series LANL. One observes a difference in the behavior of the
bursts of atmosphere glows in the red and green lines. We discuss a possible relationship ofbursts of these glows and broadband (T=0.3–600 s) geomagnetic pulsations in the postmidnight sector with the precipitation of charged particles.
THE RELATIVE ROLE OF IONOSPHERIC CONDUCTIVITY
AND ELECTRIC FIELD IN THE DYNAMICS OF FIELD-ALIGNED CURRENTS
ON THE NIGHT SIDE DURING A SUBSTORM
Vladimir Mishin, Vilen Mishin, Marina Kurikalova, Sergei Lunyushkin,Ludmila Sapronova, Yury Penskikh, Andrey Kondratev
Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
vladm@iszf.irk.ru

During the expansion phase of the magnetospheric substorm, the intensity of the fieldaligned currents (FACs) increases dramatically. There are two types of asymmetry in the
distribution of FACs in the nearmidnight ionosphere: dawn- dusk and north-south. To explainthese asymmetries, the principal scheme of the global circuit of electric currents of themagnetosphere-ionosphere (MI) system of the two hemispheres is used. Based on the output dataof the magnetogram inversion technique, the dynamics of FAC intensities in the pre- and postmidnight mesoscale cells of the three Iijima and Potemra zones, which are closed in the global
electrical circuit by meridional ionospheric currents, are analyzed. The feedback instabilities ofthe MI system are considered between the FAC intensity and: 1) the conductivity of theionosphere (type 1), and 2) the electric field (type 2). Both types of instability can operate
simultaneously in different places. The relative role of conductivity and the electric field in the
dynamics of FAC intensities during the expansion phase in the pre- and post-midnight mesoscale
cells of the summer and winter hemispheres is also investigated.

MAPPING OF IONOSPHERIC CONVECTION POTENTIAL ON POTENTIALGRADIENT FROM MULTI-STATIONS MEASUREMENTS OVER ANTARCTICA:
A CASE STUDY
Jeni Victor Nepolian, Panneerselvam C., Anil Kumar C.P., Elango P.
Indian Institute of Geomagnetism, Mumbai, India
jenivictor@gmail.com

Simultaneous observation of Potential Gradient (PG) from longitudinally (magnetic)aligned stations, Vostok (78°27 S, 106°52 E), Dome C (75°06 S, 123°20 E) and Maitri (70°45 S,
11°44 E) is presented in this work. Influence of solar wind-magnetospheric interaction on PG for
the selected geomagnetic disturbed days in the year 2010–2011is also demonstrated. Observationshows that change in Potential Gradient (∆PG) is associated with magnetic latitude during
geomagnetic disturbance. The analysis shows that small-scale changes of ionosphericelectrostatic potential (Weimer_05 model) substantially maps down at polar latitudes. For lower
magnetic latitude (Maitri), the link is evident only on severe disturbances. The linear relation (R)between PG and ionospheric potential is highly pronounced (R>~0.90) during noon-evening66

sector (06:00–18:00 UT) followed by the morning sector (00:00–06:00 UT). Nonlinear responseof PG (R<~0.3) is also accounted during midnight hours (18:00–24:00 UT) on 05–06 August
2011. The paper is also pointed out the importance of estimating PG fair-weather pattern on
monthly basis to account the ambient PG variation for every spatial station over high latitude.
GLOBAL ELECTRON CONTENT IN THE 23rd and 24th SOLAR CYCLESYury Yasyukevich1, Anna Yasyukevich1, Ilya Zhivetiev2
1
2

Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
Institute of Cosmophysical Research and Radio Wave Propagation FEB RAS, Paratunka, Russia

annpol@iszf.irk.ru

Based on the data of total electron content (TEC) Global Ionospheric Maps we analyze
behavior of the ionospheric Global electron content (GEC) in the 23rd and 24th solar cycles. We
study GEC dynamics during the 1998–2016 period as well as its annual, semiannual and 27-day
variations. We also carry out comparison of the variations parameters in GEC and regional
electron content (REC), which is the total number of electrons in the ionosphere over a certain
area, for the Baikal rift zone, European and Japan regions. The maximal amplitude of considered
REC variations is observed in Japan. Semiannual REC variations for all analyzed regions are inphase with GEC semiannual variations, while annual REC variations and GEC ones are opposite
in phase. It is shown that general dynamics of REC, GEC and their variations repeat well the
behaviour of the F10.7 solar radio emission. GEC and RECs reflect deep minimum in 2009 as
well as excess of the 23rd over the 24th one. Dependence of diurnal REC variations amplitude
on the F10.7 index is revealed to be close to linear, unlike the analogous Global electron content
dependence. The study is supported by RF President Grant of Public Support for RF Leading
Scientific Schools (НШ-6894.2016.5) and by the RFBR project No. 16-35-60018.
COMPARISON OF THE MEDIUM-SCALE WAVE ACTIVITY
IN THE IONOSPHERE OBSERVED BY THE KAZAN IONOSONDE “CYCLONE”,
DENSE GPS/GLONASS RECEIVER NETWORK IN THE MIDDLE VOLGA REGION,
AND EKATERINBURG HF RADAR
Adel Akchurin1, Alexey Oinats2, Roman Sherstyukov1
1
2

Kazan Federal University, Kazan, Russia
Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia

oinats@iszf.irk.ru

We present medium-scale traveling ionospheric disturbance (MSTID) observations using
three spatially-spaced facilities: (1) Kazan vertical sounding ionosonde Cyclone providing hightemporal resolution measurements (~1 min); (2) dense GPS-GLONASS receiver network in the
Middle Volga region (more than 200 receivers); and (3) the Ekaterinburg HF radar located near
Arti village. The ionosonde MSTID observations are carried out by analysis of vertical ionogram
features, by construction of amplitude and height maps (A- and H-maps). Dense GPS/GLONASS
receiver network allows us calculating two-dimensional maps of total electron content (TEC)
perturbation and studying dynamics of horizontal MSTID structure. The HF radar allows
registering MSTIDs by analysis of time variations of ground backscatter range associated with
HF skip distance. The facilities cover large spatial region of more than 20° along latitude andlongitude. We compare the data of these facilities in order to find similarities and differences in67

observed wave dynamics in the ionosphere and to reveal typical MSTID propagation distanceand lifetime. The work is performed according to the Russian Government Program ofCompetitive Growth of Kazan Federal University.
STUDY OF GROUND BACKSCATTER INTENSITYREGISTERED BY THE EKATERINBURG HF RADAR
Alexey Oinats1, Oleg Berngardt1, Nikolay Afanasiev2
1
2

Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
Irkutsk State University, Irkutsk, Russia

oinats@iszf.irk.ru

We present the analysis of ground backscatter intensity measured by the Ekaterinburg HF
radar (EKB radar; 56.42° N, 58.53° E) during the period from 2013 to 2016. The analysis
includes the study of the features of ground backscatter occurrence in the radar field-of-view(FOV) in order to identify specific topographic and geographic regions with enhanced/depressed
HF backscatter ability. We study diurnal and seasonal variability of ground backscatteroccurrence within the radar FOV as well as its solar and geomagnetic activity dependence. To
explain found dependencies we simulate ground backscatter intensity under different
geophysical conditions on the basis of waveguide approach. In addition we compare theobserved range profile of ground backscatter intensity with the model profile, developed in theframework of interference integral method. The advance of the model is that it determines therelation between the broadening of ground backscatter echo and the parameters of random fieldof medium-scale ionospheric irregularities. We discuss the possibility of the model application forautomated monitoring the degree of medium-scale ionospheric irregularity by use of HF radars.

COSEISMIC VERTICAL MIDSCALE IONOSPHERIC DISTURBANCES BASEDON IRKUTSK CHIRP IONOSONDE DATA IN 2011–2016
Oleg Berngardt, Natalia Perevalova, Aleksey Podlesnyi,
Vladimir Kurkin, Geliy Zherebtsov
Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
berng@iszf.irk.ru

One of the intensive sources of wave energy to the ionosphere from below are tectonic
sources. In this paper a statistical analysis is made of short-lived ionospheric effects after
earthquakes which appeared in 2011–2016 years. These effects are related with surface seismic
waves far from epicenter. We based our analysis on the Irkutsk fast monostatic chirp ionosondedata far from the epicenter and on GPS data in the epicenter vicinity.
The analysis has shown that far from epicenter some of these earthquakes wereaccompanied by vertical midscale ionospheric irregularities. To estimate the ionosphericefficiency of the seismic waves we estimated the maximal amplitude of the acoustic shock wave.
This was done by taking into account the spatial distribution of seismic vibrations and additional
acoustic wave intensification related with this.
68Based on the analysis of experimental data we have shown that earthquake-related 5–25 s.
irregularities are observed mostly at daytime at large acoustic wave amplitudes, and thiscorrelates well with case-study results from other researchers. The observations of internal
gravity waves by GPS technique in the epicenter vicinity (120–600 s irregularities) do not showsuch a daytime dependence. Possible mechanisms of this effect are discussed.
STUDIES ON VERTICAL COUPLINGS BY GRAVITY WAVES OVER
THE ANTARCTIC WITH THE GROUND-BASED OBSERVATIONS
Takuji Nakamura, Takashi S. Matsuda, Masaru Kogure, Mitsumu K. Ejiri,
Yoshihiro Tomikawa, Takaniroi Nishiyama, Masaki Tsutsumi
National Institute of Polar Research, Tokyo, Japan
nakamura.takuji@nipr.ac.jp

The high latitude southern hemisphere is known to be a region of high activity of theatmospheric gravity waves. Vertical propagation of the gravity waves is important in vertical
couplings between the troposphere, the middle atmosphere and the upper atmosphere. However,
not enough observations cover the Antarctic region to reveal such vertical couplings. Japanese
Antarctic Research Expedition (JARE) started a prioritized project of observing the middle andupper atmosphere observations in 2010. The extension of the observations included a large
MST/IS radar (PANSY radar), a Rayleigh/Raman and resonance lidar, a millimeter radiometer,
and an airglow imager. In this paper, we focus on the recent analysis results of gravity wave
observations using the sodium and OH airglow imagers and a Rayleigh/Raman lidar. The former
provides detailed information on horizontal structures of the gravity waves at 90 km altitude. The
new spectral analyses in horizontal phase velocity domain [Matsuda et al., 2014] is quite usefulin discussing the vertical propagation and the source of the internal gravity waves. The latterprovides height profiles of the inertia gravity wave activity in the middle atmosphere in detail.
This also helps to understand the generation and the vertical propagations of gravity waves indifferent aspects. These two observations have revealed the characteristics of gravity waves
around Syowa station (69° S, 40° E) and clarified a distinct difference from what has been
observed over Davis station (69° S, 78° E), about 1.500 km east of Syowa.

INTERACTION OF SMALL-SCALE GRAVITY WAVES WITH THE DIURNAL TIDEFROM THE MESOSPHERE TO THE UPPER THERMOSPHERE
Erdal Yigit1, Alexander S. Medvedev2
1
2

George Mason University, United States
Max Plank Institute for Solar System Research, United Stateseyigit@gmu.edu

Effects of subgrid-scale gravity waves (GWs) on the diurnal migrating tides areinvestigated from the mesosphere to the upper thermosphere during September equinox, using ageneral circulation model coupled with the extended spectral nonlinear GW parameterization ofYiğit et al. [2008]. Simulations with GW effects cut off above the turbopause and included in theentire thermosphere have been conducted. GWs appreciably impact the mean circulation andcool the thermosphere. They significantly affect the winds modulated by the diurnal migratingtide, in particular in the low-latitude mesosphere and lower thermosphere and in the high-latitude
thermosphere. These effects highly depend on the mutual correlation of the diurnal phases of the
GW forcing and tides: GWs can either enhance or reduce the tidal amplitude. In the low-latitude
69

MLT, the correlation between the direction of the deposited GW momentum and the tidal phaseis positive due to propagation of a broad spectrum of GW harmonics through the alternating
winds. In the Northern Hemisphere high-latitude thermosphere, GWs act against the tide due toan anti-correlation of tidal and GW phases, while in the Southern high-latitudes they weakly
enhance the tidal amplitude via a combination of a partial correlation of phases and GW-inducedchanges of the circulation. The variable nature of GW effects on the thermal tide can be captured
in GCMs provided that a GW parameterization (1) considers a broad spectrum of harmonics, (2)properly describes their propagation, and (3) correctly accounts for the physics of wave
breaking/saturation.

70

Session 4: UNDERSTANDING THE EARTH'S SPACE ENVIRONMENT
AND ITS CONNECTION TO SPACE WEATHER_____________________________________________________________MAGNETOSPHERE AND IONOSPHERE RESPONSE TO THE INTERPLANETARYSHOCK ON 24 JANUARY 2012
Vladimir Belakhovsky1, Vyacheslav Pilipenko2, Lisa Beddeley3,
Yaroslav Sakharov1, Sergei Samsonov4
1

Polar Geophysical Institute, Apatity, Russia,
Institute of the Physics of the Earth, Moscow, Russia
3
UNIS, Svalbard, Norway
4
Yu.G. Shafer Institute of Cosmophysical Research and Aeronomy, Yakutsk, Russia
2

belakhov@mail.ru

The magnetosphere and ionosphere response to the SSC event at 24 January 2012 wasinvestigated using complex of spacecraft and ground-based instruments. The SSC produce strong
increase of the energetic particles fluxes (40 keV – 2 MeV), density, temperature inside themagnetosphere as seen by the THEMIS, GOES spacecrafts. It is shown that the SSC impulse is
not shock wave in the outer magnetosphere (Mf ≈ 0.4). SSC produce the substorm developmenton the nightside during prolonged (10 hours) positive Bz-component of IMF and generation of
Pc4-5 pulsations on the morning side. We firstly show that SSC cause abrupt increase of the
TEC, determined by the GPS receivers, in the morning (ΔTEC= 20–30 %) and evening (ΔTEC≤
8–9 %) sectors of auroral zone. The increase of the TEC during SSC is not observed on the
middle and low latitudes. So obviously the TEC response is caused the particle precipitation into
the ionosphere. During the SSC the increase of the electron density at the altitudes 90–200 km
registered by the VHF EISCAT radar in Tromso. So the main contribution to TEC increase has
the lower part of the ionosphere. SSC produce strong increase of the CNA in Scandinavia and in
Svalbard. The strong increase of the aurora intensity at different spectrum lines (450–700 nm)
was registered by hyperspectral camera NARUSSCA II of the Polar Geophysical institute in
Svalbard. The SSC produce strong increase of the GIC (geomagnetically induced currents) at
electric power lines of the Kola Peninsula and Karelia (~30 A).
INVESTIGATING THE TOTAL COLUMNAL ELECTRON CONTENT RESPONSETO GEOMAGNETIC ACTIVITY AT TORO AN EQUATORIAL STATION
Rasheedat Bola Abdulrahim1, J.O. Adeniyi2
1

Department of Physics, University Of Ilorin, Ilorin, Nigeria, Nigeria National Space Research andDevelopment Agency
2
Department of Physics, Nigeria
bourlarnley@gmail.com

The study of geomagnetic storm as it affects distant radio wave transmission cannot be
overemphasized. The response of the ionospheric total electron content to geomagnetic activity
had been investigated using TEC data from a GPS system situated at Toro with geographicalcoordinates (10.12° N, 09.41° E) an equatorial region in Nigeria. The variability of theionospheric TEC during geomagnetic quiet and stormy active periods were compared. The storm
events for the period of July 6–9, November 11–17 and November 18–19, 2012 were studied.
71

The response of the Dst index was observed to be simultaneous with that of the Horizontal
component of the interplanetary magnetic Field IMF Bz and the total electron content TEC for
the July 6–9 and November 11–17 events. Both IMF Bz and Dst shows an irregular patternduring the 18–19 November event. However, there was a positive increase in the value of TEC.
There was a nighttime TEC enhancement during both main and recovery phases of the Nov 11–
17 event with percentage increase of about 23 % in the value of TEC. However, there was TEC
enhancement in the two storms studied. The observed effects during these periods could be
explained in terms ionospheric-magnetospheric dynamics as a result of modulation of theequatorial electric field by geomagnetic storms.
INTER-HEMISPHERIC FIELD ALIGNED CURRENT CHARACTERISATION
IN THE AFRICAN SECTOR AND ITS RESPONSE TO A 2009 SUDDENSTRATOSPHERIC WARMING EVENT
Oluwafisayo Paul Owolabi1, Olawale Segun Bolaji2,Jacob Olusegun Adeniyi3,
Elijah Oyedola Oyeyemi2, Babatunde Akeem Rabiu4, John Bosco Habarulema5,
Pierre Cilliers5, Lee-Anne McKinnell5
1

Space and Ionospheric Physics Laboratory, Department of Physics, University of Ilorin, Ilorin,
Kwara State, Nigeria
2
Deparment of Physics, University of Lagos, Lagos, Nigeria
3
Department of Physics, University of Ilorin, Ilorin, Kwara State, Nigeria
4
Centre for Atmospheric Research (CAR), National Space Research and Development Agency(NASRDA), Abuja, FCT
5
Science, Research and Applications Unit, South African National Space Agency, Hospital Street,
Hermanus, P.O. Box 32, Hermanus, 7200, South Africa
fisicist2009@gmail.com

The sudden stratospheric warming (SSW) is a key linkage in the vertical coupling between
the lower atmosphere and the geospace, but no studies have attempted to establish the variabilityof inter-hemispheric field aligned currents (IHFACs) in response to SSW. In this work, we
examine ground magnetic variations from September 2008 to August 2009 at eleven stations not
only to investigate IHFACs in the African chain, but also to reveal the variability of IHFACs interms of its connection with SSW. For the first time, there is a compelling evidence from ourresults that much of the IHFACs variability during the period of the winter northern hemisphere
arises mainly from SSW through the activities of planetary waves, rather than ionospheric windand conductivities or the imbalance of the ionospheric horizontal Sq current. The fact that theamplitude of the IHFACs shows an unusual depletion during this period point to a relation to theoffshoot of the 2009 SSW event. For instance, the manifestation of the latitudinal depletion in
the amplitudes of the noon time IHFACs in month of January coincides with the unusually strong
2009 SSW event. Quite unexpected, in January, a significant depletion in the IHFACs amplitude wasobserved during the noon sector around the magnetic equator (Addis Ababa, AAB), compared to any
other months under investigation, accompanied with a consistent significantly reduced amplitudes
across the Northern hemisphere and a moderate decrease in the Southern hemisphere. Other new
insights from our results are that: (1) we obtain prominent currents flowing from the Northern(summer) hemisphere to the Southern (winter) hemisphere around dusk in the equinox; (2) we obtainstrong cross – equatorial currents in the equinoxes (August and February); (3) during the noon sector,
the IHFACs in the Northern hemisphere penetrates the Southern hemisphere less deeply; and (4) the
IHFAC pattern in the African chain show a persistent reversal in the north – south asymmetry, suchthat, the ionospheric horizontal Sq current imbalance is stronger in the northern hemisphere than thesouthern hemisphere, except during the dusk. In addition, we confirm the existence of longitudinalvariations for IHFACs.
72

EFFECTS OF PENETRATING INTERPLANETARY ELECTRIC FIELD
ON THERMOSPHERIC NIGHTGLOW EMISSION VARIATIONS: A CASE STUDY
Ajesh Asokan Pillai; Vineeth Chandrashekaharan Nair; Tarun Kumar Pant
Space Physics Laboratory, Vikram Sarabhai Space Centre, ISRO, Thiruvananthapuram, Kerala,
India
india.ajesh@gmail.com

The present study reports nighttime response of the Equatorial Ionosphere Thermosphere
System (EITS) over a dip equatorial station, Trivandrum (8.5° N, 77° E, 0.5° dip lat.) to two distinct
prompt penetration electric field (PPEF) events occurred during nighttime on 05 January 2016
and 06 March 2016. The investigation carried out using the data from a Nighttime Photometer,
Digital Ionosonde, and Fluxgate Magnetometer, revealed that the thermospheric airglow (atomic
oxygen emissions) responds promptly to the PPEF events during nighttime. It has been observed
that, during the westward PPEF event, the thermospheric O1D 630.0 nm emission intensity
enhances whereas during the eastward PPEF event the intensity decreases. While the downward
transition of the ionospheric layer causes spike like enhancements in the 777.4 nm oxygen line
intensity. The behavior of ionospheric base height vindicates that during eastward (westward)
PPEF event the ionospheric layer moves upward (downward). The downward layer movement
brings more ionization to the centroid of thermospheric O1D 630.0 nm emission, which in turnenhances the emission rates. While the layer transition through the 777.4 nm emission centroid
causes the spiky enhancement on the emission. The temporal variation of emission intensities
reveals the nighttime thermospheric dynamics. This study discusses these aspects in detail.
EFFECTS OF SPACE WEATHER ON THE IONOSPHERE: A CASE STUDY OF THE
GEOMAGNETIC STORMS DURING THE PERIOD 17–28 FEBRUARY 2014
Sharon Aol
Mbarara University of Science and Technology, Uganda
sharonaol@ymail.com

Geomagnetic storms represent an extreme form of Space Weather, which can havesignificant effects on the ionosphere. This study focused on the effects of Space Weather on theionosphere during geomagnetic storms for the period 17–28 February 2014 over the African
equatorial region. The dual frequency Global Navigation Satellite System (GNSS) data were toused retrieve Vertical Total Electron Content (VTEC). Increase and decrease in VTEC comparedto monthly median VTEC represented positive and negative ionospheric storm effects,
respectively. The analysis showed that positive and negative ionospheric storm effects occurred
during the period of study. These storm effects were discussed in terms of the Prompt
Penetration Electric Field (PPEF), storm induced wind-lifting effect, and Disturbance Dynamo(DD) electric field. Occurrence of ionospheric irregularities during the storm period wasanalyzed using rate of change of TEC Index (ROTI). The results obtained show that most of thestorms studied triggered ionospheric irregularities. Furthermore, the effect of the irregularities on
GNSS signals was analyzed by determining the number of visible satellites in 30 s intervals. A
drop in the number of satellites was observed during the occurrence of ionospheric irregularities.
This suggests that ionospheric irregularities cause loss of lock in GPS receivers.
73

EFFECT OF MAGNETIC STORMS ON THE DEVELOPMENT OF SCINTILLATIONPRODUCING IRREGULARITIES IN LOW LATITUDE IONOSPHERE
Archana Bhattacharyya1, Bharati Kakad1, Padma Gurram1, Samireddypalle Sripathi1,
Surendra Sunda2
1
2

Indian Institute of Geomagnetism, India
Space Application Centre, India

abh@iigs.iigm.res.in

An important component of space weather in low latitude ionosphere is the equatorial
plasma bubble (EPB) formed by growth of the Rayleigh-Taylor instability on the bottom-side of
the post-sunset equatorial F region. As an EPB extends to the topside of the equatorial F region,
it develops structure over a wide range of scale sizes, of which the intermediate scale (~100 m –few km) irregularities give rise to fluctuations or scintillations in the amplitude and phase of
VHF and higher frequency transionospheric radio signals. The EPBs involve whole flux tubes sothat the irregularities at different altitudes over the magnetic equator map down along thegeomagnetic field lines to different latitudes. Thus ionospheric irregularities that have thepotential to degrade the performance of satellite-based communication and navigation systems
may sometimes be present in the low latitude ionosphere over a large part of the globe. Hencenumerous schemes have been developed to predict scintillations on L-band signals transmitted
from GNSS satellites. An important aspect of the development of scintillation-producing
irregularities that has not been considered in these studies is the nature of intermediate scale
irregularity spectrum at different altitudes over the magnetic equator within the much larger scale
EPB, which map to different latitudes along the geomagnetic field lines. The irregularity
spectrum as well as the background electron density determine the strength of L band
scintillations at different latitudes. Using observations of scintillations on VHF and L-band
signals recorded by a network of ground stations and modelling them using different irregularity
models, it has been recently shown that as an EPB develops over the magnetic equator, it
becomes more structured on the topside of the F region than near the equatorial F region peak.
This explains the occurrence of strong L–band scintillations near the crest of the equatorial
ionization anomaly when weak or no L-band scintillations are recorded near the magnetic
equator. Two important factors that control the development of structure in an EPB are theheight of the equatorial F region and distribution of thermospheric density which affects thealtitudinal profile of ion-neutral collision frequency. A major magnetic storm alters both throughprompt penetration of a convection or over-shielding electric field into the equatorial ionosphere,
and through the effect of a disturbance dynamo. Ionosonde and scintillation observations areused to show how the interplay of the two factors may influence the latitudinal distribution of
L-band scintillations associated with geomagnetic activity.

74THE RESPONSE OF THE IONOSPHERIC F2 LAYER PEAK PARAMETERSAROUND THE CREST OF THE EIA TO SOME SPACE WEATHER EVENTS
Jacob Olusegun Adeniyi1, Benjamin Wisdom Joshua2
12

Physics Department, University of Ilorin, Nigeria
Kebbi State University of Science and Technology, Aliero, Nigeria

benjaminjoshua7@gmail.com

The equatorial electrodynamics is known to play a vital role in the distribution ofionization at the equatorial/low latitude ionospheric region; it is responsible for the formation of
the equatorial ionization anomaly (EIA). The EIA is characterized by the formation of two crestsof ionization around ±200 magnetic latitude with a trough at the equator. This study investigates
the response of the ionospheric F2 layer over four equatorial/low latitude stations to three (twomoderate (Dst ≥ –100 nT) and one strong (Dst = –100 to –150 nT)) geomagnetic storms. Twostations were chosen on either side of the geomagnetic equator, such that they fall within thesame or a close range of local time. Results from the study show similarities in the response of
NmF2 from all the stations to the storm events; both positive and negative phases were recorded
from the two stations. The highest percentage change in NmF2 of about 86 % was recorded atJeju, South Korea, while that of the main phase (about 160 %) was recorded in Townsville,
Australia. Averagely, depletions in NmF2 dominate all the phases of the geomagnetic storms,
except the strong storm of 30 September – 01 October 2011. The main phase of this geomagnetic
storm corresponds to the daytime period in all the stations. Results from this study further
confirm the dependence of the ionospheric response during geomagnetic storms to the local time,
longitude and latitude of the stations.

ITUHAB
Furkan Ali Kucuk
Istanbul Technical University, Turkey
falikucuk@gmail.com

We have initiated a low budget project, named “ITUHAB”, that allows some high altitude
experiments at stratosphere level in Antarctica and Turkey for detecting alfa, beta and gamma
particles. The main target is launching payloads weigh less than 2.5 kg to stratosphere. We usedtemperature and humidity insulated boxes made of Styrofoam. Geiger counter air and light
pollution sensors, IR cameras which are installed in our systems can easily detect air and light
pollution. Thus, it will be possible to construct air and light pollution database in Turkey fromstratosphere level. In this study, all devices and instruments necessary for this project are GPS
modules, air and light pollution quality meters, pressure sensors, IR cameras, HD cameras andother specific sensors (i.e. temperature, humidity, radiation etc.) All tests (i.e. vacuum, very low
temperature) were performed at Istanbul Technical University Space Systems Test and Design
Laboratory. As a summary, this project will help to develop research related to space andatmospheric sciences in Turkey.

75

RECURRENT IONOSPHERIC STORMS: TEMPORAL AND SPATIAL SCALES
Alexei Dmitriev
Institute of Space Science National Central University, Taiwan, Province of China
dalex@jupiter.ss.ncu.edu.tw

Recurrent magnetic storms are produced by fast solar wind streams from coronal holes,
which co-rotate with the Sun with ~27-day periodicity. The storms accompanied by various
ionospheric disturbances of different temporal and spatial scales. The scales are related to theorigin of disturbances. We analyzed low- and mid-latitude ionospheric storms (both positive andnegative) with 2-hour resolution by using global ionospheric maps of vertical total electron
content derived from the ground based GPS network in time period from 2004 to 2009. It was
found that positive ionospheric storms have largest temporal and spatial scales: the duration can
exceed ten hours, latitudinal and longitudinal extensions can reach up to 40 and 120 degrees,
respectively. In contrast, negative ionospheric storms have ~2 time smaller scales: duration ofseveral hours, latitudinal and longitudinal extents of ~20 and 60 degrees, respectively. Various
mechanisms resulting in different temporal and spatial scales of ionospheric storms are discussed.

RESULTS FROM RADIATION ENVIRONMENT INVESTIGATIONS ON THE
INTERNATIONAL SPACE STATION IN THE PERIOD 2007–2015 WITH LIULIN-5
CHARGED PARTICLE TELESCOPE
K.N. Krastev1, J.V. Semkova1, R.T. Koleva1, C. Dachev1, N. Bankov1, S. Malchev1,
V. Benghin2
1
2

Research and Technology Institute, Bulgarian Academy of Sciences, Bulgaria
State Research Center of the Russian Federation, Institute of Medico-Biological Problems RAS,

Russiawerholak@abv.bg

The space radiation environment of the Earth is complex, composed of galactic cosmic
rays, trapped particles of the Earth’s radiation belts, solar energetic particles, albedo particles
from Earth’s atmosphere and secondary radiation produced in the space vehicle shielding
materials. Dose characteristics in near Earth and space radiation environment also depend on
many other parameters such as the orbit parameters, solar cycle phase and current helio- andgeophysical conditions. Since June 2007 the Liulin-5 charged particle telescope has been
observing the radiation characteristics in two different modules of the International Space Station(ISS). In the period from 2007 to 2009 measurements were conducted in the spherical tissueequivalent phantom of MATROSHKA-R project located in the PIRS module of ISS. From 2012
to 2015 measurements were conducted in and outside the phantom located in the Small Research
Module of ISS. In this paper attention is drawn to the obtained results for the dose rates, particle
fluxes and dose equivalent rates in and outside the phantom from the galactic cosmic rays,
trapped protons and solar energetic particle events occurred in that period. Compared are theradiation doses obtained at the deep minimum of solar activity in 23th solar cycle and close to
the maximum of 24th cycle and the implications for human space flights are discussed.

76

MANIFESTATIONS OF THE INTENSE CONVECTION AND SUBSTORM
IN THE PROTON AND ELECTRON AURORA DYNAMICS
AND IN THE SAR ARC OCCURRENCE
Igor Ievenko, Stanislav Parnikov
Yu.G. Shafer Institute of Cosmophysical Research and Aeronomy, Yakutsk, Russia
ievenko@ikfia.ysn.ru

It is known that the 486.1 nm line (H-beta) is emitted by atomic hydrogen as a result ofprecipitation of protons with the energy of ~10–20 keV and their recharging at the altitudes ofionosphere E layer (proton aurora). The red line of atomic oxygen (630.0 nm) in the aurora isradiated at the ionosphere F2 region altitudes as a result of precipitation of electrons withenergies up to ~1–2 keV. The velocity of magnetic drift of the charged particles in themagnetosphere is proportional to their energy. The energy of particles does not influence to theelectric drift. In this work, the dynamics of electron and proton aurorae in the evening MLT
sector at the Yakutsk meridian (130º E; 200° E, geom.) during the magnetic storm on January 7,2015 using the all-sky imager (ASI) is analyzed. The angular westward motion velocity of theauroral structures in the 630.0 and 486.1 nm emissions along the magnetic latitude of 58° N at ahigh value of electric field of the solar wind –VxBz = 9 mV/m (dawn-dusk) has been defined. On
the basis of this parameter the value of radial component of the convection electric field and theprecipitating protons energy have been estimated. Next, ASI data show an intensification ofaurorae in the 630.0 and 486.1 nm emissions in the range of geomagnetic latitudes of 56–61° N
and occurrence of the stable auroral red (SAR) arc at latitudes of 49–52° N in ~20 min after the
onset of an intense substorm expansion. Measurements aboard the Van Allen Probes A satellite
show a sharp increase of fluxes of the energetic Н+, О+ ions (injection boundary) at the L~2.6–3.0
at the same time near the Yakutsk meridian. The satellite registers the overlapping of energetic
ion fluxes with plasmapause in this L interval. This region is mapped by the SAR arc at lower
latitudes (L~2.2–2.6) pointing to the nondipole configuration of the geomagnetic field in the
inner magnetosphere at the current values of SYM-H ~ –120 nT and ASY-H~150 nT. The researchis supported by RFBR grants No 15-05-02372 a and No 15-45-05090 r_vostok_a.
THE JOINT ANALYSIS OF THE DYNAMICS OF THE IONOSPHERE PARAMETERS
AND COSMIC RAYS DURING PERIODS OF INCREASED SOLAR ACTIVITY
Oksana Mandrikova1, Yury Polozov1, Timur Zalyaev1, Dmitry Baishev2, Boris Shevtsov1
1

Institute of Cosmophysical Research and Radio Wave Propagation FEB RAS (IKIR FEB RAS),
Paratunka, Russia
2
Yu.G. Shafer Institute of Cosmophysical Research and Aeronomy SB RAS (IKFIA SB RAS),
Yakutsk, Russia
up_agent@mail.ru

We performed a joint analysis of the dynamics of the ionosphere parameters and cosmic
rays during periods of increased solar activity (the events for the years 2010–2016 wereanalyzed). Used computational solutions, developed by authors, are based on the application of
wavelet transform and neural networks and allows to highlight instants of occurrence ofabnormal changes in the data and evaluate their energy features. Of interest are allocatedabnormal enhancement in the intensity of cosmic rays that occur at the same time as an increasein the ionospheric electron density. Anomalous effects occurred a few hours before thebeginning of strong magnetic storms and had a large spatial and temporal scales.
77

PWING GROUND NETWORK OBSERVATION OF WAVES AND PARTICLESIN THE INNER MAGNETOSPHERE DURING THE FIRST ERG-GROUND CAMPAIGN
Kazuo Shiokawa1, *PWING Team1

Institute for Space-Earth Environmental Research, Nagoya University, Japan*Japanshiokawa@nagoya-u.jp

In order to provide global distribution and quantitative evaluation of the dynamicalvariation of plasmas and waves in the inner magnetosphere, we have started PWING Project(study of dynamical variation of Particles and Waves in the INner magnetosphere using Groundbased network observations, http://www.isee.nagoya-u.ac.jp/dimr/PWING/PWING_web_e.htm),
which will last for 5 years from April 2016, as a Grant-in-Aid for Specially Promoted Researchof the Japan Society for the Promotion of Science (JSPS). In this PWING project, we operate allsky aurora/airglow imagers, 64-Hz sampling induction magnetometers, 40-kHz sampling
ELF/VLF receivers, and 64-Hz sampling riometers at 8 stations at ~60 MLAT around the northpole, as well as two EMCCD cameras at two stations. The stations are distributed in Canada,
Iceland, Finland, Russia, and Alaska. We combine these longitudinal network observations with
the ERG (Arase) satellite, which was launched on December 20, 2016, and global modeling.
Using these comprehensive dataset, we investigate dynamical variation of particles and waves in
the inner magnetosphere, which is one of the most important research topics in recent space
physics. The inner magnetosphere contains plasmas in wide energy ranges from below electron
volts to Mega-electron volts. These plasmas (electrons and ions) interact with ULF/ELF/VLF
waves at frequencies of 0.1 Hz to 10 kHz to cause their energization in the equatorial plane of
the magnetosphere and loss into the ionosphere. The first campaign observation of PWING
project with the newly-launched ERG satellite is planned in the second half of March 2017. In
this presentation, we show PWING ground network observations of waves and particles in the
inner magnetosphere during the first ERG-ground campaign.
*PWING TEAM: Kazuo Shiokawa1, Yoshizumi Miyoshi1, Shin-ichiro Oyama1, Nozomu
Nishitani1, Kanako Seki2, Yuichi Otsuka1, Mitsunori Ozaki3, Ryuho Kataoka4, Tsutomu
Nagatsuma5, Yoshimasa Tanaka4, Iku Shinohara6, Masahito Nose7, Takeshi Sakanoi8, Fuminori
Tsuchiya8, Yuki Obana9, Shin Suzuki22, Atsuki Shinbori1, Tomoaki Hori2, Akira Kadokura4,
Keisuke Hosokawa10, Yasunobu Ogawa4, Martin G Connors11, J. Michael Ruohoniemi12, Kevin
Sterne12, Mark Engebretson13, Erik Steinmetz13, David Murr13, Esa Turunen14, Jyrki Manninen14,
Antti Kero14, Tero Raita14, Thomas Ulich14, Alexander Kozlovsky14, Arto Oksanen15, MarkoBack15, Kirsti Kauristie16, Brenton Watkins17, William Bristow17, Christopher Fallen17, Marty
Karjala17, Tyler Begley17, Marc Lessard18, Boris Shevtsov19, Igor Poddelsky19, Dmitry Baishev20,
Vladimir Kurkin21, Alexey Oinats21, Alexander Pashinin21
1
Institute for Space-Earth Environmental Research, Nagoya University, 2University ofTokyo, 3Kanazawa University, 4National Institute of Polar Research, 5National Institute ofInformation and Communications Technology, 6Institute of Space and Astronautical Science,
Japan Aerospace Exploration Agency, 7Kyoto University, 8Tohoku University, 9Osaka ElectroCommunication University, 10The University of Electro-Communications, 11Athabasca
University, 12Virginia Tech, 13Augsburg College, 14Sodankylä Geophysical Observatory,15
Nyrola Observatory , 16Finnish Meteorological Institute, 17Geophysical Institute, University of
Alaska Fairbanks , 18University of New Hampshire, 19Institute of Cosmophysical Research andRadiowave Propagation (IKIR), Far Eastern Branch of the Russian Academy of Sciences,
20
Yu.G. Shafer Institute of Cosmophysical Research and Aeronomy (IKFIA), Siberian Branch of
the Russian Academy of Sciences, 21Institute of Solar-Terrestrial Physics (ISTP), Siberian
Branch of the Russian Academy of Sciences, 22Aichi University.
78

DYNAMICS AND FEATURES OF GEOMAGNETIC DISTURBANCE PROPAGATIONDURING MAGNETIC STORMS (BASED ON GROUND STATION NETWORK)
Oksana Mandrikova1, Igor Solovyev1,2, Sergey Khomutov1,2,
Dmitry Baishev3, Kusumita Arora4, Lingala Manjula4, Phani Chandrasekhar4
1

Institute of Cosmophysical Research and Radio Wave Propagation FEB RAS, Paratunka, Russia
Kamchatka State Technical University, Petropavlovsk-Kamchatsky, Russia
3
Yu.G. Shafer Institute of Cosmophysical Research and Aeronomy, SB RAS, Yakutsk, Russia
4CSIR-National Geophysical Research Institute, Hyderabad, India
2

kamigsol@yandex.ru

Geomagnetic data for the periods of magnetic storms in 2015 (events on January 07,
March 17, June 21–22, August 15, and December 19–20) were analyzed. The data were recordedat the stations located along a meridian in the north-east of Russia (Kotelny KTN, Tixie TIX,
Chokurdakh CHD, Zyryanka ZYK, Cape Shmidt CPS, Yakutsk YAK, Magadan MGD,
Paratunka PET, Khabarovsk KHB) and at near equatorial Indian stations (Hyderabad HYB and
Choutuppal CPL). A method developed by the authors was used to detect local increases ingeomagnetic disturbance intensities and to estimate their dynamic characteristics. Small-scale
short-period increases of geomagnetic activity were detected and analyzed. They occur
simultaneously at all the stations under analysis several hours before the beginning of thegeomagnetic storms. During the main phase of the storm, the areas of activation were detected which
had large spatial scales and, evidently, associated with the processes of energy accumulation andrelief in the magnetosphere. The development of the method was supported by RSF Grant No.14-1100194. Experimental investigations were supported by RFBR Grant No. 16-55-45007.
SHORT-TIME FORECASTING OF THE MID-LATITUDE TOTAL ELECTRONCONTENT WITH A MEDIAN MODEL AND A FOURIER TRANSFORMATIONAPPROACH
Ronny Badeke, Claudia Borries
German Aerospace Center (DLR) Kalkhorstweg 53/17235 Neustrelitz, Germany
Ronny.Badeke@dlr.de

Predictions of the ionosphere are important information for users for either mitigation of
threats due to ionospheric perturbations or for the purpose of mission planning. However,increasing uncertainties for forecasts of more than one hour can limit the usability of forecasts.
Here, users may have individual thresholds. Therefore, we present an estimation of the accuracyof quiet time forecasts to allow judgement of their applicability and identification ofdevelopment needs. Empirical prediction of the quiet-time ionospheric total electron content(TEC) is performed with two time-series approaches: the Median Model (MediMod) and a
Fourier Transformation approach. Time-series models calculate their prediction values out of themost recent data or maps. The models are applied on real-time map values of the Space Weather
Application Center Ionosphere (SWACI). The forecast accuracy is presented for 1 day, 3 days,
7 days and 27 days forecasts ahead and in a comparison between medium and high solar active
during the years 2011 and 2015, respectively. A decreasing accuracy of longer forecasts andduring higher solar activity is apparent as expected. We will show the definite values todemonstrate the performance of both approaches.
79ACCELERATION OF THE ELECTRONS TO THE RELATIVISTIC ENERGIES AT
THE OUTER RADIATION BELT DURING MAGNETIC STORMS AND WITHOUT IT
Vladimir Belakhovsky1, Vyacheslav Pilipenko2, Laura Simms3,
Mark Engebretson3, Sergey Samsonov4
1

Polar Geophysical Institute, Apatity, Russia
Institute of the Physics of the Earth, Moscow, Russia
3
Augsburg College, Minneapolis, MN, United States
4
Yu.G. Shafer Institute of the Cosmophysical Research and Aeronomy, Yakutsk, Russia
2

belakhov@mail.ru

It is considered traditionally that the appearance of relativistic electrons is one of the
manifestations of the magnetic storms in the near-Earth environment. Here we present someevents showing that the rate of the electron flux increase does not depend on the geomagnetic
storm intensity and such increase can even occur without geomagnetic storm. Using themagnetic field and charged particle data from the GOES geostationary satellites the accelerationof the electrons with energies from 40 keV to > 2 MeV in the outer radiation belt is investigated.
To characterize the magnetospheric wave activity in the Pc5 frequency range (1–7 mHz) the
ULF index is used. The electron fluxes with lower energies start to grow earlier than fluxes ofsubrelativistic and relativistic electrons. The necessary condition of the electron acceleration to
the relativistic energies is a prolong substorm activity which is accompanied by the injection ofseed electrons (50–100 keV), generation of VLF waves, and the occurrence of the high speed
solar wind streams promoting the Pc5 wave generation. The correlation between the periods withthe high solar wind speed and growth of the relativistic electron fluxes with a 1–2 days delay
confirms the idea about the important role of the drift resonance of the magnetospheric electrons
with MHD waves in the Pc5 frequency range. The resonant interaction between them leads to theelectron radial diffusion deep into the magnetosphere and their preliminary acceleration up to thesubrelativistic energies.

CHARACTERING THE GEOMAGNETIC FIELD VARIABILITY FOR THE STUDY
OF MAGNETIC STORM AND SUBSTORM IMPACT ON ELECTRIC POWER LINES
Vyacheslav Pilipenko1, Vladimir Belakhovsky2,
Yaroslav Sakharov3, Vasiliy Selivanov2
1Geophysical Center, Moscow, Russia
Polar Geophysical Institute, Apatity, Russia
3
Institute of the Physics of the Earth, Moscow, Russia
2

belakhov@mail.ru

The geomagnetically induced current (GIC) intensity is determined by variations ofgeomagnetic field. Predominantly geomagnetic field disturbances are oriented in the N–S
direction, and produced by the E–W ionospheric currents. Thus, such disturbances seemingly
will not induce any significant GIC in a latitudinally oriented system. However, during magnetic
storms GIC in power systems elongated in the N–S direction were quite significant. The relative
contribution of geomagnetic disturbances into GIC enhancements are examined using data from
GIC-recording system deployed by Polar Geophysical Institute. We apply to the IMAGE
80

magnetometer data for the geomagnetic storm 17 March 2013 various techniques to characterize
the geomagnetic field variability: vector mapping of time series, and a measure of time variationsof vector angle cosines. This technique has shown that ionospheric currents fluctuate not just in
E–W direction, but chaotically in both E–W and N–S directions. So these fluctuations cannot be
described only by variations of the auroral electrojet intensity but the model of the GIC
estimation must take into account small scale current systems in the ionosphere.

PROCESSES IN THE FRONT OF BOW SHOCK
Pavel Sedykh
Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
pvlsd@iszf.irk.ru

The front of the bow shock (BS) is the region where the parameters of the solar wind (SW)undergo strong changes, especially in the nose part. The particle number density and theintensity of the tangential component of the magnetic field increase approximately by a factor of
4 behind the front, the normal velocity component decreases by the same factor (according todata of well-known satellite missions: GEOTAIL, CLUSTER-II, THEMIS; interplanetary shocks
in SPECTR-R). If almost all SW energy before the front is concentrated in the progressive
motion, then behind the front it is concentrated in the energy of compressed gas and magnetic
field. The bow shock front is the main converter of solar wind kinetic energy into
electromagnetic energy (Ponomarev, Sedykh et al., 2006). When passing through the bow shock
front, the intensity of the tangential component of the SW magnetic field and the plasma density
increase several fold. Therefore, among other things, the BS front is a current sheet. It is possible
to show that current is diverging in this layer, i.e. the front is the generator of the electric current.
Since plasma with magnetic field passes through the front, electric field arises in the front
reference system. Thus, the BS front is a source of electric power. There is a potential difference
between the BS front and the magnetosphere, unequivocally (since the magnetic field ofmagnetosheath or transition layer (TL) is determined by the SW magnetic field) associated withthe velocity of the transition layer plasma flow. Thus, the magnetopause potential is functionallyrelated to SW parameters. The power consumed by the magnetosphere is spent on thecompressor work and consists of active and reactive power. The active part covers losses in theionosphere (ohmic, primarily), the reactive part returns to the magnetospheric compressor(Sedykh 2011; Sedykh and Ponomarev 2012). We shall assume the bow shock front to be aparaboloid of rotation with its axis coinciding with the X axis in the solar-magnetosphericcoordinate system. In the paper we shall be limited to a simple case – I shall consider the
dependence only from coordinate x. Certainly, more full decision of the general problem (whendependence not only on one coordinate is examined) has to be considered. However, it is notpossible to solve at once a complex problem analytically. Therefore in this study we shall belimited to such statement of a problem. Further, the obtained solution can be generalized on moredifficult cases. It is clear that the primary energy source for magnetospheric processes is the solar
wind, but the process of energy transfer from the solar wind into the magnetosphere, or rather, toconvecting magnetospheric plasma, appears to be rather complicated. The solar wind energy also
feeds the ion acceleration process, the generation of waves in the region of bow shock, and theenergy necessary to build up the foreshock.

81

SUBAURORAL ION OUTFLOW WITHIN POLARISATION JET
Artem Gololobov1, Alexander Stepanov2, Viktor Khalipov3,
Innokenty Golikov2
1

North-Eastern Federal University, Yakutsk, Russia
Yu.G. Shafer Institute of Cosmophysical Research and Aeronomy, Yakutsk, Russia
3Space Research Institute, Moscow, Russia
2

golart87@gmail.com

Polarisation Jet, or SAID, is a narrow band of fast westward convection which can appear
during magnetic storms in the subauroral zone approximately along the nightside plasmapause. It
causes strong heating of subauroral plasma due to collisions, fast plasma outflows, and ion conic
formation. It results at F-region altitudes in upward or downward plasma motions, a narrow drop
in density, or trough in the trough, changes in ion composition, an electron temperature peak,
weak SAR-arc, density inhomogeneities and other effects. Data on ion drifts and field-aligned
ion outflows from Kosmos-184 and DE-2 satellites at ionospheric altitudes are analysed. Modelcalculation have shown that bi-Maxwellian ion distributions resulting from perpendicular ion
heating in regions where the magnetic field is inclined to the satellite velocity vector, can produce
vertically asymmetric fluxes in a driftmeters frame which mimic fast field-aligned ion flows. It isshown that in many cases the data within the Polarisation Jet are consistent with the contribution of
the perpendicular ion heating as an additional cause of the observed fast convection.

MODELING THE FORMATION OF HOT RING ZONE IN THE SUBAURORALIONOSPHERE IN WINTER
Artem Gololobov, Innokenty Golikov, Ilya Varlamov
North-Eastern Federal University, Yakutsk, Russia
golart87@gmail.com

The modeling results of electron temperature distribution in F region of the subauroral
ionosphere for different helio-geomagnetic conditions considering plasmaspheric heat fluxes arepresented. The study has been conducted using a three-dimensional model of high-latitude
ionosphere in Euler variables in view of its thermal regime. It is shown that for quiet geomagnetic
conditions during a winter period in the dawn and dusk sectors the “hot” zones with the higher
electron temperature are formed, and for disturbed geomagnetic conditions an annular “hot” region
in the time interval of 04–06 UT is formed as a result of heat flow from the Earth’s plasmaspherealong the magnetic field lines. Analysis of data obtained with the DE-2 and CHAMP satellites
shows the possibility of formation of such zone during geomagnetic disturbances.

82

PRECIPITATION OF RELATIVISTIC ELECTRONS UNDER CYCLOTRONRESONANT INTERACTION WITH ELECTROMAGNETIC ION-CYCLOTRONWAVESVeronika Grach1, Andrei Demekhov2
1
2

Institute of Applied Physics RAS, Nizhny Novgorod, Russia
Polar Geophysical Institute, Apatity, Russia

blackrookg@gmail.com

We study cyclotron resonant interaction of relativistic electrons in the Earths radiation
belts with ion-cyclotron waves. Wave packets with varying frequency are considered, and thedipole model of geomagnetic field is used. The equations describing the interaction of test
particles with a given wave packet are solved numerically. We analyze the results of numericalsimulations for a large number of test particles and obtain the probability of electron trapping
and the probability of significant change in electrons pitch-angle for both trapped and untrappedelectrons. The energy and pitch-angle variation in the trapping and untrapped regimes are studied
for relativistic electrons of outer radiation belt. Conditions, under which effective electron
scattering into the loss cone is possible, are obtained and analyzed. It is shown that, depending
on electron energy, the interaction with a wave-packet of a constant amplitude can be both more
and less efficient than the interaction with a wave-packet having a varying (Gaussian-shaped)
amplitude. We compare the results with the numerical simulations reported previously by otherauthors and with current experimental data.

TEC VARIATIONS OVER MEXICO OBTAINED WITH TAYABSTEC METHODMaria Sergeeva1, Olga Maltseva2, Juan Americo Gonzalez-Esparza1,
Victor Jose Gatica-Acevedo3
1

SCiESMEX, Institute of Geophysics, Universidad Nacional Autonoma de Mexico, Morelia.
CONACYT, Instituto de Geofisica, Universidad Nacional Autonoma de Mexico, Morelia
2Institute for Physics, Southern Federal University, Rostov-on-Don, Russia
3
Instituto Politecnico Nacional, Mexico City
maria.a.sergeeva@gmail.com

Total electron content (TEC) is one of the main parameters characterizing the Earth’s
ionosphere. The study presents the analysis of TEC variations over the territory of Mexico. At
the moment there is no available ionospheric sounding data in the country. Consequently, TEC
studies have a special value for estimating the ionosphere state in this region, especially during
Space Weather disturbances. Developed networks of GNSS receivers in Mexico (TLALOCNet
and SSN) provide the opportunity of continuous TEC monitoring in near-real time. From 2015
this monitoring is performed by the Mexican Space Weather Service (SCiESMEX). TEC values
for this study were derived from data of local GNSS receiver stations with use of TayAbsTEC
technique designed by Institute of Solar-Terrestrial Physics, Siberian Branch, Russian Academyof Sciences. The results were compared to global ionospheric maps. The benefits of the
TayAbsTEC data processing method for Mexico region were shown. In particular, TayAbsTEC
allowed us to observe the finer TEC deviations (small-scale effects). The data during different
quiet and disturbed geomagnetic periods between 2011 and 2016 was studied. Regular patterns83

(diurnal, seasonal, annual) of TEC behavior over Mexico were obtained which include
dependence on solar activity, shift of the main diurnal maximum to the afternoon hours, night-time
TEC enhancements, annual anomaly and winter anomaly presence. The results were compared topatterns of other low-latitude zones. Specific features of TEC behavior during disturbances werediscussed. An important peculiarity for Mexico was revealed: the presence of strong positive TEC
enhancements sometimes not related to geomagnetic disturbances is characteristic for this region.
The results were confirmed by measurements at low-altitude satellites.

PREMIER INVESTIGATION OF THE OCCURRENCE FREQUENCY
OF EQUATORIAL PLASMA BUBBLES OVER NIGERIA USING THE ALL-SKY
OPTICAL IMAGER AND GNSS OBSERVATIONS
Akeem Babatunde RABIU1, A. Babatunde Rabiu1, Daniel I. Okoh1, K. Shiokawa2,
E.O. Falayi3, O.S. Bolaji4, E.O. Oyeyemi4, R.O. Kaka5, S.E. Onwuneme6
1

Centre For Atmospheric Research, National Space Research And Development Agency, Kogi
State University, Anyigba, Nigeria
2
Center for International Collaborative Research (CICR), Institute for Space-Earth Environmental
Research (ISEE), Nagoya University, Furo-cho, Chikusa-ku, Nagoya, Aichi, 464-8601, Japan
3
Tai Solarin University of Education, Ijagun, Ijebu Ode, Nigeria
4
Department of Physics, University of Lagos, Akoka, Nigeria
5
Afe Babalola University, Ado-Ekiti, Nigeria
6
University of Port Harcourt, Port Harcourt, Nigeria
tunderabiu2@gmail.com

The work examined the frequency of occurrences of plasma bubbles and the seasonal
dependence over an African equatorial region using the All-Sky Optical Imager and GNSS
observations. The All-Sky Optical Imager, situated in Abuja, has about 500 km fish-eye view
covering almost the entire airspace of Nigeria (Longitude 2–15° E and latitude 4–14° N). The
GNSS receiver stations used are those within the coverage of the all-sky imager. To enhance thevisibility of plasma bubbles on the images, image analysis was performed on the raw images bycomputing 30-min running mean deviations for the images. Data for the period of June 2015
(when the imager was installed) to January 2017 was used. The images were observed on a dayto-day basis to identify whether or not plasma bubbles were recorded. Computations ofdifferences between evening-time and day-time ROTI (Rate of change of TEC Index) were also
used to decide whether or not plasma bubbles were observed on the GNSS observations.
Observations from the two sets of equipment were fairly consistent. Preliminary results from thestudy reveal that there are more plasma bubble occurrences over the region during the months ofMarch and April (March Equinox months) and less occurrences during the months of December
and January (December Solstice months).

84

SUBSTORMS OBSERVED DURING GEOMAGNETIC STORMS BY THE CAMERASSYSTEM MAIN IN APATITY
Veneta Hristova Guineva1, Irina Despirak2, Boris Kozelov2, Rolf Werner1
1

Space Research and Technology Institute (SRTI), Stara Zagora Department, Bulgarian Academyof Sciences, Stara Zagora, Bulgaria
2
Polar Geophysical Institute (PGI), Apatity, Russia
v_guineva@yahoo.com

In this work substorms generated during geomagnetic storms were examined. Observations
from the Multiscale Aurora Imaging Network (MAIN) in Apatity during 2024/2015, 2015/2016
and 2016/2017 winter seasons have been used. Solar wind and interplanetary magnetic fieldparameters were taken from the 1-min sampled OMNI data base. Substorm onset and further
development were verified by the 10-s sampled data of IMAGE magnetometers and by data of
the all-sky camera at Apatity. Subject of the study were the substorm peculiarities during
different storm phases. A statistical study of the substorm auroras development depending on thelevel of geomagnetic activity expressed by the SYM/H and AE geomagnetic indices was carriedout and discussed.
STORM TIME ION COMPOSITION VARIATIONS IN THE NEAR EARTH PLASMASHEET USING SPACE BORNE MEASUREMENTS
Megha Mahendrabhai Pandya1, B. Veenadhari1, Masahito Nosé2, Sandeep Kumar1,
Geoffrey Reeves3
1

Department of Science and Technology, Indian Institute of Geomagnetism, Navi Mumbai, India
Data Analysis Center for Geomagnetism and Space Magnetism, Graduate School of Science,
Kyoto University, Kyoto, Japan
3
Space Science and Applications group at Los Alamos National Laboratory, Los Alamos, New
Mexico, United States
2

megha.pandya14@gmail.com

Streaming solar wind particles and ionospheric O+ ions play an important role in the global
dynamics of the Earth’s magnetosphere. The major particle source for the plasma sheet ions issolar wind and ionosphere. The ion composition of the near-Earth plasma sheet changes with thegeomagnetic conditions. The solar wind ions contributes the most to the plasma sheet population
during geomagnetically quiet conditions while, ionosphere contributes exclusively during thegeomagnetic storm conditions. Its ion composition change during different interplanetaryconditions is compared using energetic particle flux data obtained from Geotail spacecraft and
Van Allen probes. Intense and moderate geomagnetic storms from solar cycle 23 and 24 with ioncomposition variations in the near-Earth plasma sheet are compared. Intense geomagnetic storms
shows higher O+/H+ and He+/H+ energy density ratio than the moderate ones while there is astrong geomagnetic storm dependence on singly charged heavy O+ ions. The energy density of
H+, O+ and He+ ions also depends on the magnitude and duration of southward IMF Bz andsolar wind dynamic pressure. The ion composition changes in plasma sheet are comparable to
the ring current region, as reported in previous studies indicating transport of ionospheric ionsfrom plasma sheet to the ring current region through mass dependent acceleration by convection
electric field. Some of the results regarding the intense and moderate events for solar cycle 23
and 24 will be discussed in the meeting.
85

DYNAMICS OF THE PROTON AURORA AND SAR ARC
ACCORDING TO THE ALL-SKY IMAGER DATA AS THE MAPPING OF PC1 WAVE
EASTWARD PROPAGATION ALONG THE PLASMAPAUSE
Igor Ievenko, Stanislav Parnikov, Dmitriy Baishev
Yu.G. Shafer Institute of Cosmophysical Research and Aeronomy, Yakutsk, Russia
ievenko@ikfia.ysn.ru

The stable auroral red (SAR) arcs are the consequence of interaction of the plasmapause
with energetic ions of the ring current. The Pc1 waves are registered on the Earth as aconsequence of generation of electromagnetic ion cyclotron (EMIC) waves in the equatorial
plane of the magnetosphere. EMIC instability causes the scattering of ring current protons into
the loss cone. Precipitation of energetic protons and their recharge on the heights of theionosphere E layer can be observed as a proton aurora in the H-beta line of atomic hydrogen. In
this work the dynamics of the SAR arc, proton aurora and Pc1 waves in the MLT evening sector
at the Yakutsk meridian (130° E; 200° E, geom., MLT midnight is 15:50 UT) using the all-sky
imager (ASI) and induction magnetometer during the growth and expansion of intense substorms
on December 31, 2015 is analyzed. After the enhanced magnetospheric convection due to thesouthward IMF Bz turning ASI observes an equatorward motion of the diffuse aurora (DA)boundary in the 557.7 and 630.0 nm emissions and H-beta (486.1 nm) band from the northernhorizon of observation station. The weak SAR arc is registered equatorward of DA since thebeginning of observations. During the expansion phase with the onset at ~12:12 UT and epicenter inthe midnight MLT sector the SAR arc center is located at the geomagnetic latitude of 58° N at thezenith of the station. The band in the H-beta emission is registered at the latitudes of 59–61° N. In 10
minutes after the start of substorm expansion ASI registers the SAR arc intensity growth from thewestern horizon toward the east with an angular velocity of ~4 deg/min. As a result, along the arc a
few intensity maxima are formed. At the same time, the narrow band in the H-beta emission with asimilar dynamics appears poleward of the SAR arc at a distance of ~ 0.6°. The induction
magnetometer detects a sharp increase of Pc1 pulsation amplitude during the arrival of end of theband in the H-beta emission to the zenith of observation station. The Pc1 pulsations and the dynamic
proton aurora are registered within ~ 30 min. The SAR arc is registered by ASI until about 1400 UT.
We connect the observed phenomena in the SAR arc and proton aurora with the propagation processof EMIC waves to the east along the plasmapause. The generation of EMIC waves occurs probably
at higher L shells in the boundary region of plasmaspheric plume. The research is supported by
RFBR grants No 15-05-02372 a and No 15-45-05090 r_vostok_a.
EXPERIMENTAL STUDY OF THE PLASMASPHERE BOUNDARY LAYER
Galina Kotova1, Mikhail Verigin1, Vladilen Bezrukikh1, Joseph Lemaire2
1
2

Space Research Institute of RAS, Moscow, Russia
Universite Catholique de Louvain, Faculty of Science, Louvain-la-Neuve, Belgium

kotova@iki.rssi.ru

The boundary of the plasmasphere – the plasmapause – is a crucial place for the interaction ofenergetic particles with the cold plasma. Many specific phenomena are observed in this region:
development of Polarization Jet (SAID, SAPS), Subauroral red arcs, formation of Subauroral
morning proton spots etc. During large magnetic storms the plasmapause approaches L~2.5 and thering current energetic particles are observed close to the Earth at such distances, and this is essential
86

for the space weather safety studies. The in situ cold plasma measurements onboard MAGION 5
were carried out with very good time resolution and permitted to analyze thin boundary layer near
the plasmapause. It is found that in this layer the plasma density NPBL is decreasing exponentiallywith L: NPBL~exp(-L/WPBL), where WPBL describes the width of the plasmasphere boundary
layer. The density in the middle of the boundary layer is inversely proportional to the volume ofmagnetic flux tube, whereas its width is proportional to the volume of magnetic flux tube. The widthof the boundary layer also depends on magnetic activity and on time elapsed since the most recent
burst of magnetic activity. The talk is partially supported by the program 1.7 P of RAS.
ANALYTIC MODEL OF CHANGES IN THE MAGNETOPAUSE SHAPE
AND POSITION WITH IMF AND SOLAR WIND PARAMETERS VARIATIONS
Mikhail Verigin, Galina Kotova, Vladilen Bezrukikh
Space Research Institute RAS, Moscow, Russia
verigin@iki.rssi.ru

It is generally accepted to use solar wind ram pressure and IMF Bz component for
empirical description of the geomagnetopause position and shape. Specific feature of the present
talk is to use not solar wind parameters but neighboring to magnetopause thermal, and magnetic
field pressures for proper modeling. These pressures are deduced basing on the results of 3D MHD
runs and analytic solutions for post bow shock MHD flow in Lagrangian variables. IMF By and Bz
components influence the planetary magnetopause position and shape in two different ways: bothcomponents lead to increase close to magnetopause magnetic pressure while Bz part of IMF leads
additionally to variation of this boundary shape. The magnetopause shape variation in turn changes
the so called ‘doubling factor’ which indicates how much the internal magnetospheric field isincreased due to Chapman-Ferraro currents. Doubling factor can be analytically related withmagnetopause shape by Tsyganenko magnetospheric field ellipsoidal model. Incorporating all above
effects in our analytical model leads to ‘perfect’ description of ‘rapid’ magnetopause approach to the
Earth for southward IMF and to its ‘stagnative’ behavior with increase of northward IMF component.
Our analytic model well describes additionally the magnetopause motion with variation of IMF coneangle. The talk is partially supported by the program 1.7 P of RAS.
CORRECTION OF THE NeQuick MODEL AT HIGH LATITUDES USING GROUNDBASED GNSS RECEIVERS - VERIFICATION BY IONOSONDE DATA
AND HF RAY TRACING
Daria Kotova1,2, Vladimir Ovodenko3, Yury Yasyukevich4, Igor Nosikov1,2,
Maxim Klimenko1,2
1West Department of Pushkov IZMIRAN, RAS, Kaliningrad, Russia
Immanuel Kant Baltic Federal University, Kaliningrad, Russia
3
Joint Stock Company Scientific Research Institute of Long-Distance Radio Communication,
Moscow, Russia
4
Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
2

Darshu@yandex.ru

In recent years, attention to investigation and diagnostic of ionosphere significantly
increases. This is largely due to the fact that the requirements for the radio systems accuracy
87using ionospheric channel is increased significantly. Consequently high accuracy of ionosphericmodeled prediction and/or real-time definition is required. Nowadays, global navigation satellite
system (GNSS) such as GPS and GLONASS, worldwide ground-based network of satellite
signal receivers provide a new possibility of real time ionospheric monitoring. GNSS Signal
Processing is used for calculating absolute total electron content (TEC) along radio path between
each satellite and ground-based receiver. However, integral nature of absolute TEC parameter
causes difficulties for real application. Absolute slant TEC can be used for the correction ofionospheric models providing more accurate electron density distribution. In this paper, we
propose modeling of HF ray tracing in the high-latitude ionosphere. To describe the electron
density of the propagation medium the correction of absolute TEC data from NeQuick model isused. Correction algorithm of ionospheric model parameters is based on the control parameters
according to the slant TEC. Smoothed sunspot number R12 in the NeQuick is an example ofsuch parameter. The number of the parameters requiring for the calculation of the complex
refractive index for the ordinary and extraordinary waves, were taken from empirical IRI model.
In addition HF ray tracing modelling is performed by the shooting method and direct variational
approach. Simulation of ray paths was provided for all seasons and time of day in 2014. These
calculations were carried out by two methods: variational method, and homing-in approach. We
compared the calculation results and the experimental data in order to estimate the efficiency of
the algorithm for ionospheric model correction according to slant TEC data adaptation.In recent
years, attention to investigation and diagnostic of ionosphere significantly increases. This islargely due to the fact that the requirements for the radio systems accuracy using ionosphericchannel are increased significantly. Consequently high accuracy of ionospheric modeledprediction and/or real-time definition is required. Nowadays, global navigation satellite system(GNSS) such as GPS and GLONASS, worldwide ground-based network of satellite signal
receivers provide a new possibility of real time ionospheric monitoring. GNSS Signal Processing
is used for calculating absolute total electron content (TEC) along radio path between eachsatellite and ground-based receiver. However, integral nature of absolute TEC parameter causes
difficulties for real application. Absolute slant TEC can be used for the correction of ionosphericmodels providing more accurate electron density distribution. In this paper, we propose
modeling of HF ray tracing in the high-latitude ionosphere. To describe the electron density ofthe propagation medium the correction of absolute TEC data from NeQuick model is used.
Correction algorithm of ionospheric model parameters is based on the control parameters
according to the slant TEC. Smoothed sunspot number R12 in the NeQuick is an example ofsuch parameter. The number of the parameters requiring for the calculation of the complex
refractive index for the ordinary and extraordinary waves, were taken from empirical IRI model.
In addition HF ray tracing modelling is performed by the shooting method and direct variational
approach. Simulation of ray paths was provided for all seasons and time of day in 2014. These
calculations were carried out by two methods: variational method, and homing-in approach. We
compared the calculation results and the experimental data in order to estimate the efficiency of
the algorithm for ionospheric model correction according to slant TEC data adaptation. The
reported study was funded by RFBR according to the research project No. 16-35-00590 мол_a.

88

FORMATION OF HIGH DENSITY REGIONS IN THE PLASMASPHERE BY
VERTICAL FLUXES OF COLD IONS FROM THE IONOSPHERE
Victor Khalipov1, Galina Kotova1, Mikhail Verigin1, Alexander Stepanov212Space Research Institute RAS, Moscow, Russia
Yu.G. Shafer Institute of Cosmophysical Research and Aeronomy, SB RAS, Yakutsk, Russia

khalipov@iki.rssi.ru

Cold plasma measurements onboard the INTERBALL spacecraft reveal the regions in theplasmasphere where the density was 3–5 times higher than in the neighbor regions. Such regions
were mostly observed after the substorm activations. Ground based and satellite measurements in
the ionosphere during substorms, showed that fast upstreaming plasma fluxes are formed in thepolarization jet band. The vertical velocity of such fluxes achieves 1.0–1.5 km/s at the height of
DMSP satellites (~850 km). The case study comparing the observed high-density structures in
the plasmasphere with high speed plasma streams from the ionosphere during the polarization jet
development, taking into account the time of plasma transport from the ionosphere to theplasmasphere, reveals the interconnection of these phenomena. The talk is partially supported by
the program 1.7 P of RAS.
EXPERIMENTAL STUDIES OF PHYSICAL CONDITIONSFOR THE POLARIZATION JET FORMATION
Victor Khalipov1, Alexander Stepanov2, Elena Bondar2
1
2

Space Research Institute RAS, Moscow, Russia
Yu.G. Shafer Institute of Cosmophysical Research and Aeronomy SB RAS, Yakutsk, Russia

khalipov@iki.rssi.ru

Observations of polarization jet (PJ) by the coherent backscattering radar – SuperDARN –in Tasmania showed that PJ is developing during the substorm break up. These observations
confirm the conclusion made previously from the data of Yakutian chain of ionosondes. This fact
is very important for the analyses of possible mechanisms of PJ formation. The SuperDARN
data also evidences on the existence of large sporadic electric fields at the moment of PJ
formation, and this suggests that thermoelectric mechanism of electric field creation in the modeof voltage generation is effective. The connection of PJ with the injection of ions into the innermagnetosphere is considered in details using simultaneous measurements by the ionosonde chain
and onboard AMPTE/CCE. It is shown PJ is formed on the ionospheric projection of the innerinjection boundary of ions with the energy of 20–30 keV. According to ground-based
measurements on the longitude chain of ionospheric stations the velocity of westward motion of
the source responsible for the PJ formation is 3 hours MLT per hour at L=3. This corresponds tothe velocity of azimuthal drift of ions, observed by AMPTE/CCE. The mechanism of PJ
generation should be effective even in the conditions of high electrical conductivity in sunlit
summer ionosphere. In the region of PJ formation due to strong heating of neutrals under theaction of electric field, the thermospheric circulation is completely reconstructed.

89

EXPOSURE TO EXTERNAL INFLUENCES EARTH АND SOLAR SYSTEM
Gennady Smolkov
Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
smolkov@iszf.irk.ru

The study and attempts to explain the properties so-called Solar-Terrestrial Relations werein a protracted crisis. Without taking into account the roles and contributions of all external
influences on the Earth still has not explained their mechanisms and cyclicity, energetics, polar
asymmetry, synchronicity, and others species of manifestations. Answers to these questions are
obtained by taking into account, in addition to solar activity and the flow of GCR, theendogenous activity of the Earth due to the gravitational influence from the Moon, the Sun andthe other planets in the barycentric motion of the Solar system in the gravitational field of the Galaxy,
as well as external influences on the Solar system whole. Taking into account all the external factors
allowed explaining a pause or a temporary reduction in global warming in 1998–2013.
ON NON-UNIVERSALITY OF SOLAR-TERRESTRIAL CONNECTIONS
Lev Aron Pustilnik
Israel Cosmic Ray and Space Weather Center, Tel Aviv University & Israel Space Agency &Golan Research Institute, Israel
levpust@post.tau.ac.il

Non-universality of the solar-terrestrial connection (STC) caused by complex anddynamical character of the dynamo process in the Sun from the one side and of the non-stabilityof the global atmospheric circulation in the Earth from the other side. These reasons lead fromtime to time to drastically change of the STC manifestations as whole. Partly it leads to changeof the phase relations between different forms of the Earth environment responses (EER) on
solar activity (SA). The dynamo mechanism, controlled SA, includes few basically elements(differential rotation, solar convection, toroidal and poloidal magnetic fields, global circulationand more). All this elements are connected one to another with direct and feedbacks causalreason relations between them. In result solar cycle has dynamically change in amplitude, inperiod and in phase behavior up to phenomena of strange attractor. This non-stationarity leads todifferent phase pattern of main manifestations of solar activity and its non-stability (sunspots
number, flares frequency (with different phase patterns for different amplitudes), coronal holes,
chromosphere emission and more). When this non-stability overlaps on non-stability of the
global atmospheric and oceanic circulation, it leads to complex and non-stable response of theearth weather and climate on solar activity. We discuss this non-universal character of STC andits sequences for identification of solar variability in atmospheric, agriculture response and wheat
price dynamics. We propose list of necessary conditions and possible scenarios of SCT taking inaccount the non-universality of SCT.

90RESPONSE OF HIGH FREQUENCY RADIO WAVE PROPAGATIONCHARACTERISTICS TO THE X-RAY FLUX VARIATIONS
Vera Ivanova1, Sergey Ponomarchuk1, Aleksey Podlesnyi1, Zinaida Dumbrava2,
Aleksey Poddelsky2
1
2

Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
Institute of Cosmophysical Research and Radio Wave Propagation FEB RAS, Paratunka, Russia

moshkova@iszf.irk.ru

In this work we carry out the analysis of HF radio wave propagation characteristics
obtained over several paths located in the Siberian and Far Eastern regions of Russian Federation
during periods of solar flares from C to X classes by X-ray fluxes data. The lowest observed
frequencies (LOF) have been evaluated using program complex of automatic interpretation of
oblique-incidence sounding (OIS) ionograms. We analyze OIS data obtained from 2014 till 2016
LOF values characterize signal absorption over the paths. LOF variations for studied days werecompared with LOF median values for the month investigated. Sharp LOF increases during
studied X-ray solar fluxes in comparison with quiet conditions were registered over all paths. In
the moment of maximum of X-ray fluxes disappearance of reflections from lower layers of
ionosphere has been observed, HF signals propagation has occurred by means of reflections fromF2 layer. Amplitude of HF signal has been decreased also. Thereby as a result of our study of HF
radio wave propagation characteristics response to the X-ray flux variations sharp increase ofradio waves absorption and decrease of frequency range during solar flares has been observed.
The modeling of HF radio waves propagation characteristics on the base of complex algorithm
which includes modules of ionosphere and plasmasphere global model and radio waves
propagation model for the several solar flares has been carried out.
TEC ENHANCEMENT IN SOUTHERN HEMISPHERE DURING MAGNETIC STORMOF AUGUST 15, 2015
Ilya Edemskiy1, Jan Lastovicka2, Dalia Buresova2, John Bosco Habarulema3
1

Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
Institute of Atmospheric Physics CAS, Prague, Czech Republic
3
SANSA Space Science, Hermanus, South Africa
2

ilya@iszf.irk.ru

Solar flare of August 14, 2015 caused strong magnetic storm and significant increaseelectron density at the lighted side of the Earth. This enhancement is clearly observed at Global
Ionospheric Maps (GIM) and has separated pronounced areas of high density. The mostinteresting is the one located in high latitudes of Southern Hemisphere. We investigate thephenomenon in details using different sounding instrument and facilities in the region and tried
to explain the mechanism of its generation.

91

FORCING OF COSMIC RAYS ON THE EARTH’S ATMOSPHERE
Alexei A. Krivolutsky
Central Aerological Observatory, Russia
krivolutsky@mail.ru

The way to understanding the mechanisms of cosmic influence on the atmosphere of the
Earth has a rather long history. In the 70th of XX century on the basis of theoreticalinvestigations it was found, that energetic particles coming from space (solar and galactic cosmicrays) create new HOx and NOx chemical compounds, which destroy ozone in catalytic cycles.
After that new mechanism was used in model photochemical simulations. In XXI century it
became possible to compare the results of model simulation with satellite observations (UARS,ENVISAT). The results of model simulations, which illustrate the response of chemicalcomposition (neutral and ionized) and dynamics of the atmosphere to major solar proton eventsare presented. Changes in electron density induced by galactic cosmic rays are also presented.
THE DRIFT-COMPRESSION WAVES PROPAGATING IN THE EASTERNDIRECTION
Danila Kostarev
Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
kostarev@mail.iszf.irk.ru

In the work in the gyrokinetic framework it was shown that in the magnetosphere the driftcompression waves can be propagating in the drift direction of energetic electrons. The plasma isassumed to be composed of core cold particles and a hot admixture of protons with a Maxwell
distribution and electrons with an inverted distribution. The conditions of existence of such waves
and their amplification due to resonance interaction with energetic electrons (drift instability) havebeen found. The obtained results can be useful for interpretation of wave observations in themagnetosphere with frequencies in the range of geomagnetic pulsations Pc5 and below.
ANALYSIS OF TECHNIQUE FOR PLASMA TEMPERATURES DETERMINATIONON THE BASIS OF RADIOPHYSICAL MODELOF INCOHERENT SCATTER SIGNAL
Viktor Tashlykov, Andrey Medvedev
Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
vtashlykov@iszf.irk.ru

Irkutsk incoherent scatter radar (IISR) enters to the world net of ground-based instruments
for ionosphere remote sensing. These instruments may be considered to be basic for ionosphereindirect measurements in the wide range of altitudes. As any incoherent scatter facility, the IISR
construction is unique, what necessitates special technical approach to determination of plasma
parameters under study. IISR raw data (in terms of quadrature independent realizations) arebeing kept on HDs. This allows to save the all information that signal may contain. Hence, if theprocessing technique was not very correct, we could improve it using comprehensive approaches
to systematical errors counted out. The most effective approach on the basis of theory is the92direct model of backscattered signal. The following sources of systematical errors are understudy: 1. Time integration of independent realizations and effects of radio noise. 2. The IISR
radiates and receives signal of linear polarization. So power profiles of the received signal havedying-outs because of Faraday Effect. This leads to complication of ambiguity function that
couples statistical performance of plasma fluctuations with that of the received signal. 3. Spectral
distortions are treated in terms of physical phenomena they reflect. Doppler shift determines thevalue of neutral wind velocity along the radar beam. Complicated symmetric form of the spectra
depends on ion composition. Spectral asymmetry may be explained whether by presence ofelectric fields unexpected in middle latitudes or by peculiarity of radar construction – frequency
scanning (dependency of radar pattern direction form operating frequency). 4. Significant
contribution of coherent component to backscattered signal is experimentally observed. The
main assumption for nature of this component is integral contribution of plasma turbulence with
its own spectra. A technique for its estimation is under development. The goal of this study is toprovide regular high-quality estimations of plasma temperatures for Siberian region.
Acknowledgement The study was done under RF President Grant of Public Support for RF
Leading Scientific Schools (NSh-6894.2016.5). Experimental data was obtained with uniquescientific equipment Irkutsk incoherent scattering radar, reg. nb. 01-28. The work was done
under the basic research project II.12.2.1 Development of new methods for experimental
radiophysical studies of the upper atmosphere of the Earth and near-Earth space.
SIMULTANEOUS OBSERVATION OF RADIO SIGNAL IONOSPHERIC SCINTILLATIONS IN METER AND DECAMETER BANDS IN THE DIRECTION OF THE
MAGNETIC ZENITH
Mariia Globa, Roman Vasilyev, Yury YasyukevichInstitute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
globa@iszf.irk.ru

Radio signal scintillations in the ionosphere occur due to scattering on irregularities, whose
size is close to size of first Fresnel zone for signal frequency. In the number of papers it was
shown that intensity of radio signal scintillations increases when line of sight (LOS) to the sourceof radio signal and geomagnetic field vector become almost collinear. This effect is usuallyreferred to as magnetic zenith effect and believed to be caused by field-aligned irregularities ofionosphere plasma density (FAIs). Scintillations in direction of magnetic zenith were observed
using facilities of ISTP SB RAS observatory of atmospheric radio probing – Irkutsk incoherent
scatter radar (IISR) and Novatel GPStation-6 receiver. IISR operates in 154–162 MHz frequency
band, and navigation signal receiver – at ~1.2 and ~1.6 GHz. For this study we used dataobtained at IISR from June18 to July 1, 2015. During this experiment IISR operated in passivemode without transmitting any signal, as a radio telescope registering cosmic radio noise. Thismode allows to measure the power of discrete radio source Cygnus-A emission with high time
resolution (4.5 seconds) and to investigate fast radio signal amplitude variations using
scintillation index S4 and also to perform their spectral analysis. GPS/GLONASS receiver allows
to measure both amplitude (S4) and phase scintillations with 1 min resolution. The analysis ofdynamic spectra of Cygnus-A emission scintillations under quiet geomagnetic condition has
shown substantial widening of amplitude spectrum when the source approaches magnetic zenith.
This causes increase in S4. During geomagnetic storm on June 22, 2015 disturbances wereobserved away from the magnetic zenith and their amplitude spectrum differed from the quiet
one significantly: sharp increase of scintillation intensity was observed in wide band during mainstorm phase. The navigation receiver data analysis shows no dependence of amplitude93

scintillation intensity at ~1.2 and ~1.6 GHz on angle between LOS and geomagnetic field, but
we have found the clear dependence for phase scintillations. Also we have studied correlations
between amplitude and phase scintillations of the navigation signal in decameter band andamplitude scintillations of Cygnus-A emission in meter band for the same ionosphere area.
Acknowledgements The study was done under RF President Grant of Public Support for RF
Leading Scientific Schools (NSh-6894.2016.5) and supported by the Russian Foundation for
Basic Research (project N 15-05-03946_a). Experimental data was obtained with uniquescientific equipment Irkutsk incoherent scattering radar, reg. nb. 01-28. The work was done by
the basic research project II.12.2.1 Development of new methods for experimental radiophysicalstudies of the upper atmosphere of the Earth and near-Earth space.
COMPARISON BETWEEN CALIBRATED AND ABSOLUTE POWER
MEASUREMENTS AT THE IRKUTSK INCOHERENT SCATTER RADAR
Artem Setov, Andrey Medvedev, Victor Tashlykov
Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
artemsetov@gmail.com

Incoherent scatter (IS) radars are most informative instruments for regular measurementsof ionospheric parameters including height profiles of electron density, ion and electron
temperatures, plasma drift velocity, ion mass and collision frequency. Irkutsk Incoherent Scatter
Radar (IISR) is horn antenna 246 × 12.2 m with polarization filter that limits transmission andreception to a linear polarization. This limitation together with frequency range 154–162 MHz
leads to fading of the received signal due to Faraday rotation in the ionospheric plasma. By
following phase of the fading, one can restore height profile of electron density without
considering exact power levels. This method was utilized at IISR during long-term observations.
There is radar equation that links electron density of the ionosphere and power measured by theradar. This work is dedicated to comparison between absolute IS power, obtain with Faraday
rotation method, and actual measured power. Inequality between the two may be referred to an
additional scatter, reflection or absorption in the atmosphere. The results allow us to validate
Faraday rotation method and improve our estimations of electron density, plasma temperatureand drift velocity since any unaccounted coherent signal affects them. To accomplish thecomparison, we have performed calibration of receiving channels using extraterrestrial sources —we convolved sky temperature map based on Global Sky Model with antenna radiation pattern
and used it as source of known signal. Using regression between measured and known noise weestimated total gain and system noise for the radar. Several other peculiarities like compensation
for bias and nonlinearity of antenna frequency response also should be taken into consideration.
Apart from ionospheric measurements, calibration of receiving channels helps to evaluate signals
from passive observations of the Sun. Acknowledgement The study was done under RF
President Grant of Public Support for RF Leading Scientific Schools (NSh-6894.2016.5).
Experimental data was obtained with unique scientific equipment Irkutsk incoherent scatteringradar, reg. nb. 01-28. The work was done under the basic research project II.12.2.1“Development of new methods for experimental radiophysical studies of the upper atmosphereof the Earth and near-Earth space”.

94

STATISTICAL CHARACTERISTICS OF FLASHES IN THE ATMOSPHERE BASEDON CCD PHOTOMETER DATA
Ivan Tkachev, Roman Vasilyev, Alexander Mikhalev, Stepan Podlesny,
Artem Setov
Institute of Solar-Terrestrial Physics SB RAS, Russia
tid007@mail.iszf.irk.ru

Fast dynamic optical processes in the upper atmosphere of the Earth can be divided into
phenomena associated with atmospheric electricity, phenomena caused by magnetosphereionospheric interaction through particle precipitation, and phenomena associated with meteors
and artificial satellites of the Earth. In addition, we can note optical flashes associated withsuperhigh-energy subatomic particles invading the Earth atmosphere. According to the latest
information, transient light phenomena (Transient luminous Events, TLE) such as sprites, elves,
halos, giant jets are connected to the region of thunderstorm activity. A global picture of thelocation of these geophysical events is that they predominantly occur in the equatorial zone. The
first registration of fast optical flashes with a multichannel zenith photometer and an analysis of
the results obtained by means of the geophysical observatory of the ISTP SB RAS were carriedout in 2000. Estimations of the luminosities of optical flashes for various ranges of the optical
spectrum, the distribution over durations, and the probability of recording optical flashes during
the night were obtained. Comparison of the moments of registration of optical flashes andgamma-ray bursts was carried out according to the data of the BATSE catalog. The extremely
low occurrence frequency of TLE over the central parts of the continents of the northern andsouthern hemispheres, particularly in Eurasia, in conjunction with the observed rapid optical
flashes, raises the question of the nature of the flashes or the refinement of the results obtained.
At the end of November in early December 2016, night sky monitoring was resumed for the
searching of fast optical flashes using a photometer based on a CCD matrix. The using ofmodern devices based on CCD matrix with a time resolution of a few seconds makes it possible
to determine the local space morphology of events which are the reason of the fast optical flashes
in the Earths atmosphere, and for the selection of fast optical flashes from meteors. In this work
we use a photometer based on a CCD matrix designed to observe fast processes (units ofseconds). The photometer is assembled on the basis of the SONY ICX285AL CCD matrix (video
camera-285 / P-USB, development of the NGO VIDEOSKAN, http://videoscan.ru/). As an input
lens is used the lens Jupiter 3. Resolution (pixels) 1392×1040. Pixel size (μm) 6.45×6.45. Matrix
size (inch / mm) 2/3 (8.77×6.6) Exposure time from 3.5 microseconds to 110 seconds. The frame
frequency (Hz) is from 7.7 to 19.5. The working spectral range is 400-800 nm. Observations are
conducted on the territory of the Geophysical Observatory Торы (51.809813° N, 103.077429° E)
of ISTP SB RAS. The camera is mounted on a fixed mount at an angle of ~ 51° to the horizon
and directed to the north. Exposure time of 2 seconds was chosen based on preliminary results ofthe photometer work. The main objective of the study is to determine the cameras capabilities for
fixing fast optical flashes, artificial Earth satellites and meteor bolides. The results ofobservations for December 2016, January and February 2017 are revived in the paper. An
automatic algorithm for selecting a frame with a flash is described. Automated algorithms for
extracting frames containing satellites and meteor bolides are proposed. Based on the primary
flash database, a statistical analysis of the results was carried out. The contribution of naturalnoise is estimated. The study was done under RF President Grant of Public Support for RF
Leading Scientific Schools (NSh-6894.2016.5). The data of the CCD of a photometer included in
the optical complex of the CCU «Angara» were used in the work. The work was carried out withthe financial support of the project Study of dynamic processes in the system of a neutral
atmosphere — the ionosphere — the Earth’s magnetosphere. Unique number is 0344-2014-0006.
Reg. Number Center for Information Technologies and Systems-01201281656. The internal
cipher of the Institute is 200 005 100.
95

THE PATTERN OF IONOSPHERIC DISTURBANCES CAUSED BY COMPLEXINTERPLANETARY STRUCTURE ON 19–22 DECEMBER 2015
Vladimir Kurkin, Nelya Polekh, Nina Zolotukhina
Institute of Solar-Terrestrial Physics SB RAS, Russia
kurkin@iszf.irk.ru

On 19 December 2015 a heliospheric structure created by two interplanetary coronal massejections (ICMEs) triggered two-step severe geomagnetic storm. It started at 16:17 UT on 19
December, reached a first minimum of SYM-H = –77 nT at 09:20 UT and a peak intensity –170 nT
at 22:52 UT on 20 December. The initial phase was associated with an upstream sheath of ICMEs;
first step, with ~ –16 nT interplanetary magnetic field (IMF) Bz component and ~30÷70 cm–3 solar
wind density(Nsw); second step, with IMF Bz decrease from –10 to –19 nT and solar wind
rarefying from 50 to 2 cm-3. The high Nsw does not allow to identify the mentioned negative
IMF Bz regions as magnetic clouds. The recovery phase developed during southward IMF Bz
weakening on the background of Nsw ~2 cm–3. An analysis of ionospheric disturbances was
conducted using ionospheric data obtained in Northern hemisphere near meridian 120° E. During
the initial phase an increase in F2 layer critical frequency (foF2) was detected only at the mostequatorward Hainan station (19° N) nearby midnight. The foF2 increase was preceded by agrowth of F2 layer peak height by about 100 km coincident with a sharp northward IMF Bz
turning, thus with reduction of magnetospheric convection and generation of eastward overshielding electric field. During the first storm’s step the stations located northward of 25° N
observed positive foF2 disturbance which could be associated with amplified equatorward
thermospheric wind caused by high-latitude Joule heating. It was the most intensive at lowlatitude Okinawa station. The second step was characterized by blanketing sporadic Es layers at
high latitudes, an absence of clearly defined disturbances at middle latitudes, and fluctuating
increased foF2 at low latitudes. At the beginning of the recovery phase fluctuating increased foF2
appeared at 30–40° N. At low latitudes wave-lake fluctuation of decreased foF2 were observed
up to the end of the phase. The fluctuations of foF2 were similar to those of polar cap PCN/PCS
indices, but there is no one-to-one correspondence between their phases. The long-duration foF2
depletion which could be associated with thermospheric composition changes was observed onlyat high-latitude stations. This work was supported by RFBR grant N 16-05-00563.

ANALYSIS OF FINE STRUCTURE OF BACKSCATTERED SIGNALSBASED ON EKB ISTP SB RAS RADAR DATA
Ivan Lavygin, Valentin Lebedev, Konstantin Grkovich, Oleg Berngardt
Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
lavygin@mail.iszf.irk.ru

Coherent decameter (8–20 MHz) radar EKB ISTP SB RAS works in monitoring mode. Its
field-of-view covers an approximate segment Ekaterinburg — Norilsk — Novaya Zemlya. The
basis of radar operation is transmitting sounding sequences and receiving both the signals
backscattered by ionospheric irregularities (ionospheric scatter, IS) and signals backscattered by
the Earth’s surface irregularities (ground backscatter, GS). Analysis of the average parameters of
the scattered signal — Doppler frequency shift (DFS), spectral width and scattered power, allows
96such radar to investigate processes in high- and mid-latitude ionosphere. Statistical methods ofthe scattered signal processing are developed well enough. In this work, a preliminary analysis of
the fine structure of the backscattered signal had been made. Based on the model of single
scatterers, which had been initially designed for VHF Irkutsk Incoherent scatter radar, thealgorithm for analyzing the scattered signal was made. The model signal is a superposition ofelementary signals similar to the transmitted, with different amplitudes, DFS and the initial phase.
These parameters are determined from experimental data. We used three criteria of the signal
presence: the minimum of the phase root-mean-square deviation (RMSD) to the linear phase
trend, the maximum of the correlation function (CF) between received and model signal, and theminimum RMSD between the quadrature components of received and model signals. The resultsfor each method were used to construct the statistical distributions of DFS, signal/noise ratio andphase RMSD. A comparative analysis of the different scattering types was performed based on thesestatistical distributions. The analysis has shown that the distributions are very similar for IS and GS.
The difference between the distributions of IS/GS and noise looks substantial. This makes theseparation of noise from IS/GS possible even for individual samples of scattered signal.
STORM TIME OCCURRENCE OF THE IONSPHERIC TROUGH
IN GPS-TEC MEASUREMENTS OVER EUROPE
Irk Shagimuratov, Galina Yakimova, Ivan Efishov, Nadezhda Tepenitsyna,
Luiza Koltunenko, Olga Borchevkina
1West Department of Pushkov Institute of Terrestrial Magnetism, Ionosphere and Radio Wave
Propagation RAS, Kaliningrad, Russia
shagimuratov@mail.ru

In the dynamics of the main ionospheric trough during December 20, 2015 storm in TEC(Total Electron Content) is presented. The active phase of the storm started on December 20,
2015 after midnight. Maximal value of Sum of Kp reached of 45, maximal value of Dst was
about –155 nT near 23 UT. Recovery phase of storm took place December 21, 2015. For
analyses of trough the TEC latitudinal profiles formed from TEC maps over Europe have beenused. GPS observations collected by International GNSS Service (IGS) and European Permanent
Network (EPN) were used to create TEC maps. More than 150 stations from Europe were
included in the analysis. The dense world-wide GPS network provided TEC measurements withhigh spatial resolutions. The TEC maps over Europe are presented at http://data.
wdizmiran.ru:8080. High-precision phase measurements were used while processing. After preprocessing an absolute TEC for all satellite-receiver paths was calculated. In order to obtain thespatial and temporal variation of TEC and to create TEC maps, the measurements were fitted to aspherical harmonic expansion in a geographic latitude and longitude. The large number of GPS
stations in Europe provides good coverage for GPS data and enable high-accuracy TEC maps
with a temporal resolution of 5 min to obtain. The profiles were created with resolution of 1
degree at fixed longitude of 20° E. An automatic procedure was developed to identify the troughsignatures. To locate the trough mimima we used the criterion of the curvature for TEC function.
A visual identification was used to control and check the automatic procedure. Usually thetrough signatures on latitudinal profiles are demonstrated as the minimum values of TEC withwell-defined equatorial and polar walls. During winter the trough-like structure can berecognized in evening and night hours. During the storm the sharp decrease of TEC, which was
associated with the trough, was recognized in daytime after 13 UT. Location the troughminimum was evaluated near 66° N. After 13 UT a trough minimum shifted toward equator
97

untill 51 N. In this time it was recogized seconf trough minimum located near 68° N. The troughstructure can recognize as occurrence of high latitude trough. During recovery of phase storm thebehavior of TEC profiles similar one main phase of storm, but latitudinal location of trough takeones stand at higher latitudes. In whole latitudinal profiles during storm demonstrate morevariability against quiet conditions. This investigation was supported by RFBR Grant N 16-0501077, partly Program N 7 of the Presidium RAS.

FABRY—PEROT INTERFEROMETER KEO SCIENTIFIC ARINAE FOR AIRGLOWOBSERVATION IN THE EASTERN SIBERIA: FIRST RESULTS
Roman Vasilyev, Alexandr Mikhalev, Irina Medvedeva, Geliy Zherebtsov,
Alexander Beletsky, Tatyana Syrenova
Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
roman_vasilyev@iszf.irk.ru

We present measurements technique and first results obtained with the Fabry—Perot
Interferometer (FPI) which was recently installed at the Geophysical Observatory of the Instituteof Solar-Terrestrial Physics (51.8° N, 103.1° E, Tory). Using FPI measurements data we canderive neutral wind and temperature at the height of emission layers. The instrument has someindividual technical features which allow us to observe upper atmosphere airglow from several
spectral regions and obtain data on various atmospheric emissions including OI 630 nm and OI
557.7 nm. The input window of the instrument is equipped by the electromechanical periscopewith automatical operation. So, we can organize any observational program (timing anddirection) during the night. Moreover, using modern bandpass filters and CMOS chamber withcooling and thermal control for all thermally sensitive parts provides the powerful tool for upper
atmosphere study. In the present work we describe the modification of the method for retrievingline position and width from observed interferogramms. Using proposed method we obtainednight variations of neutral wind and temperature from 630 nm (~250 km) and 557.7 nm (~97 km)
emission data. The obtained results were compared with reference models of the upper
atmosphere and with the results obtained from other existing observational tools installed at the
ISTP Geophysical Observatory. At the moment we can conclude that temperature values derived
from 630 nm oxygen line data are in agreement with existing empirical model of the airglow but
lower than ones calculated using MSIS model. The neutral winds velocities obtained from 630 nm
and 557.7 nm emission data are mostly in agreement with HWM-14 model for MLT andthermosphere. The work was performed with equipment of collective usage area “Angara”. The
work was carried out with the financial support of the project Study of dynamic processes in thesystem of a neutral atmosphere — the ionosphere — the Earths magnetosphere (Unique number
is 0344-2014-0006, Reg. Number CITiS-01201281656), and RF President Grant of Public
Support for RF Leading Scientific Schools (NSh-6894.2016.5).

98

ABOUT OBSERVATIONS OF SPECTRAL RESONANCE STRUCTURESIN THE FREQUENCY BAND OF THE ALFVEN IONOSPERIC RESONATOR
AT THE MAGNETIC STAION BAYGAZAN
Alexey Gvozdarev1, Evgeniy Utchaikin1, Alexandr Kolmakov2, Sumer Kelyuev1
1
2

Gorno-Altaysk State University, Gorno-Altaysk, Russia
Tomsk State University, Tomsk, Russia

gvozdarev@ngs.ru

In November 2014, an induction magnetometer developed by the Gorno-Altaysk State
University (GASU) based on the INT-1 sensor (provided by the Institute of Solar-Terrestrial
Physics of the SB RAS) was installed at the magnetic station Baigazan of the GASU andmonitoring of geomagnetic variations was started. The low level of magnetic noise at the station,
which is located on the cordon of the Altay Reserve, and the relatively high sensitivity of theequipment allows us to confidently register the spectral resonance structures (SRS) in thefrequency band of the ionospheric Alfven resonator and three Schumann resonances (8, 14, 20 Hz).
A preliminary analysis of the frequency of observations of the SRS at the station for 2015–2016 was
conducted. The dynamic spectra for induction magnetometer data, were calculated and, according to
the characteristic patterns of the SRS, the days of their observations were revealed. SRS wasobserved at night. The one-year period wave for number of SRS observation per month with aminimum in the summer months (1–5 obs/month) and maximum in the November (20 obs/month)
have been identified. The average percentage of SRS observation days at the station is 35 %.

HIGH-ENERGY MAGNETOSPHERIC ELECTRONS DURING LAST SOLAR CYCLESOlga Kryakunova1, Anatoliy Belov2, Artem Abunin2, Maria Abunina2, Sergei Gaidash2,
Irina Tsepakina1, Nikolay Nikolayevskiy1
1Institute of Ionosphere, Almaty, Kazakhstan
Pushkov Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation RAS,
Moscow, Russia
2

krolganik@yandex.ru

The daily fluence of electrons is selected as the main characteristic of the behavior ofelectrons with energy >2 MeV measured by GOES satellites in geostationary orbit, since thischaracteristic is closely related with malfunctions of satellite electronic equipment. It is shownthat the increases in the flux of high-energy magnetospheric electrons are associated withconsiderable interplanetary and magnetospheric disturbances, but the beginning of the electron
increases lags behind them by 1–3 days. A greatly increased solar wind speed is observed as 3 days
before the electron flux starts to grow, with a maximum being reached by onset of growth. It isshown that the electron fluence is weakly associated with the level of geomagnetic activity on
the same day, but correlates to Ap-index of geomagnetic activity observed 2–3 days earlier. The
fluence of high-energy magnetospheric electrons is closely associated with the solar wind speed,
especially with its value measured 2 days earlier.

99

INVESTIGATION OF ACTIVE AREA DYNAMICS IN AURORAL ZONE USINGOBSERVATIONS OF IRREGULAR GEOMAGNETIC PULSATIONS
Iurii Lipko, Ravil Rakhmatulin, Aleksandr Pashinin
Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
lipko@iszf.irk.ru

The analysis of middle latitude Pi2 irregular geomagnetic pulsation during auroral
substorms in various longitudinal sectors of Russian Arctic was carried out. In particular, thebehavior of the main axis of polarization ellipse of irregular geomagnetic pulsation wasinvestigated. The technique of determination substorm longitude in auroral zone using theobservations of irregular pulsations in middle latitudes was offered. Data was obtained onmagnetometric complex «Angara» of Institute of solar-terrestrial physics SB RAS. More than 50
magnetic disturbances were analysed. The main axis of polarization ellipse of middle latitude Pi2
irregular geomagnetic pulsation indicate dynamics of auroral active areas.
ON THE ROLE OF PLASMA SHEET STATE IN THE MAGNETOSPHERIC PLASMAACCELERATION BY THE SOLAR WIND
Nikita Stepanov, Viktor Sergeev
Saint Petersburg State University, Saint Petersburg, Russia
nekit098@gmail.com

A well-known substorm-related plasma acceleration in the magnetosphere, launched by thearrival of southward IMF and dayside reconnection is considered as a primary magnetosphericacceleration process, which leads to the precipitation of the electrons into ionosphere, changing
its conductivity and ionospheric currents. Less appreciated is that the state of solar wind plasma
controls the background plasma sheet parameters, which themselves influence the acceleration ofmagnetospheric plasma. Based on 19 years long data base of EISCAT observations in
Scandinavia and THEMIS database, we investigate statistically the ionospheric conductivity
variations, and how they are influenced by the plasma sheet and solar wind state. We find thatthe main solar wind drivers for AL index, Pedersen and Hall conductances are the SW merging
electric field (e.g., Kan-Lee function, Ekl) and the solar wind velocity Vsw, however thehierarchy of SW drivers varies. Whereas Ekl is the main driver of AL index, the role of Vsw
increases for the conductances so that it outruns the Ekl as main driver for the Hall conductance.
We explain this by the action of some additional, solar wind velocity dependent, acceleration
mechanism, that increases the energy of the precipitated electrons. Recently the importance of
solar wind control was discussed in relation to the chorus wave acceleration (which provides the
population for the radiation belts), as well as to the intensity of field-aligned electrostatic
acceleration (contributing to the ionospheric conductivities and ground magnetic perturbations),
which both depend on plasma sheet electron parameters Te and Ne proportionally to eTN =(Te)1/2/Ne. In this talk we are trying to show how the plasma sheet state, influences the energy ofelectrons precipitated, due to magnetospheric plasma acceleration influenced by the solar wind.

100

REAL-TIME MODIFICATION OF OVATION-PRIME-PC MODEL: VALIDATION
AND NOWCASTING
Alexander Nikolaev1, Vera Nikolaeva1, Oleg Troshichev1, Patrick Newell2
1
2

Arctic and Antarctic Research Institute (AARI), Saint Petersburg, Russia;
Johns Hopkins University, Applied Physics Laboratory, Laurel, Maryland, USAdemosfen.spb@gmail.com

OVATION-Prime model is based on spectral measurements of auroral particles (electrons
and ions) onboard DMSP spacecraft and parameterized by solar wind driving. Distinguishingfeatures of the model include the separation of aurora into categories (diffuse aurora,monoenergetic, broadband, and ion), the inclusion of seasonal variations, and separate parameter
fits for each MLATxMLT bin, thus permitting each type of aurora and each location to havediffering responses to season and solar wind input. To predict auroral power far better than Kp orother traditional parameters, the model uses an optimized solar wind — magnetosphere coupling
function (dФMP/dt) which is defined by parameters measured at the Lagrange point (L1).
However, when using dФMP/dt, some difficulties may arise: (1) in the case, when the solar wind,measured by ACE spacecraft in L1, is not encountered with the magnetosphere at all, (2)dependence of the precipitating particles distribution on magnetospheric conditions (under thesame conditions in the solar wind the magnetospheric response may be different). These
problems are automatically eliminated if we examine 1-min PC index as a current electric field
EKL actually impacting the magnetosphere, and replace coupling function dФMP/dt with PC
index. The PC-index as a quantitative characteristic of the substorm activity level can essentially
improve timing within substorm cycle that in turn allowed us to compare observable aurora
dynamics (e.g. captured by THEMIS all-sky cameras or Polar spacecraft) with those computedby modified OVATION-Prime model. We use PC-index to (1) eliminate the need for solar windparameters as model input and (2) applied it to develop real-time PC-based version of
OVATION-Prime model.
GROUND-BASED SUPPORT OF SATELLITE MISSIONS AT KOLA PENINSULA
Boris Kozelov
Polar Geophysical Institute, Apatity, Russia
boris.kozelov@gmail.com

Last decades a numerous satellite missions aimed to study the response of the Earths space
and atmospheric environment to solar drivers have been realized and are still planning.
Successful use of the international near-Earth satellite mission data depends largely upon the
ground-based observations in conjugate regions. The high-latitude regions have a key role insuch observations as regions where varied processes in the magnetosphere, ionosphere, andatmosphere are the most prominent. The observatories of Polar Geophysical Institute located at
Kola Peninsula can give important additional eastward extension of the Scandinavian groundbased support of the satellite missions. In this report we review the available equipment andpossible data of the optical, VLF/ULF and other measurements. Capabilities and potential resultsof the coordinated observational campaigns are discussed on the examples of conjugations with
Van Allen Probes and THEMIS satellites.

101FORECASTING OF GEOEFFECTIVENESS AND COSMIC RAY MODULATIONINDUCED BY COROTATING INTERACTION REGIONS
Jaša Čalogović1, Mateja Dumbović1, Bojan Vršnak1, Bernd Heber2, Manuela Temmer3,
Astrid Veronig3
1

Hvar Observatory, Faculty of Geodesy, University of Zagreb, Kačićeva 26, 10000 Zagreb, Croatia
Institute for Experimental and Applied Physics, Christian-Albrechts-University Kiel, Germany
3Institute of Physics, University of Graz, Universitätsplatz 5, A-8010 Graz, Austria
2

jcalogovic@geof.hr

When high-speed solar wind streams originating in coronal holes (CH) interact with thepreceding slow solar wind, they form regions of compressed plasma called “corotatinginteraction regions” (CIR). These phenomena can influence Earths space environment, cause thegeomagnetic storms and modulate the cosmic rays (CR) flux at the Earth. With the aim to
improve space weather predictions, we investigated the relationship between the area of CHs anddifferent geomagnetic indices corresponding to equatorial (Dst, ring current), middle (ap) andhigh (AE, polar electrojet) latitude regions. The relationship between CH area and CR flux using
satellite CR measurements taken from SOHO EPHIN was also studied. The minimum phase of
the solar cycle 23–24 (2007–2010) was selected for analysis due to lower CME activity. Since
the interplanetary near-Earth disturbances are delayed about 4 days after the changes in CH area,
this gives a good opportunity to forecast a CR modulation on Earth and geoeffectiveness of CIRs.

GEOEFFECTS OF CHELYABINSK METEOROID ENTERING THE EARTH’S
MAGNETOSPHERE
Yury Lipko, Ravil Rakhmatulin, Aleksandr Pashinin
Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
lipko@iszf.irk.ru

On 15 February 2013, a superbolid having a diameter of about 17 m and a mass of about
17,000 t entered the Earth’s atmosphere at a velocity of about 18 km/s. At 03:20:33 UT, it
exploded over Chelyabinsk, at a height of 22 km. After the fall of the Tunguska meteorite on
30 June 1908, it has been the second largest cosmic body entering the Earth’s atmosphere in thepast 100 years. A 17,000-tonne block of stones, metal and ice passed through all layers of the
Earth’s upper atmosphere (magnetosphere, plasmasphere and ionosphere). If we assume that
passage of this cosmic body in the Earth’s magnetosphere was geoefficient, then the desired
signal had to be detected after the body entered the Earth’s magnetosphere, 80–60 min before theexplosion in the atmosphere. According to the analysis of AU, AL, AO and Kp indices, the bolide
passed the Earth’s magnetosphere under very quiet magnetic conditions. Induction
magnetometers at the ISTP SB RAS station for registering geomagnetic pulsations (the Republicof Buryatia, the Eastern Sayan, φ=51.4°, λ=100.5°) and at the IKIR FEB RAS Geomagnetic
Observatory “Paratunka” (Kamchatka, φ=53.1°, λ=158.4°) showed a noise-like burst invariations of the magnetic field in the frequency range 0.2–5 Hz at 02:45–02:58 UT (i.e., 35 min
before the meteoroid explosion). The anomaly registered at mid-latitude observatories underquiet geomagnetic conditions could be due to the interaction between the meteoroid and theEarth’s plasmasphere. According to the review of papers dealing with occurrence of magnetic
effects during the passage and explosion of the Tunguska meteorite in the Earth’s magnetosphereand atmosphere on 30 June 1908, some researchers noticed anomalies in variations of thegeomagnetic field 80 min prior to the explosion.
102Session 5: SUN TO EARTH CAMPAIGN EVENT STUDY_____________________________________________________________
CHALLENGES IN UNDERSTANDING AND PREDICTING EARTH-AFFECTING
CORONAL MASS EJECTIONS
Nariaki Nitta1, Tamitha Mulligan2, Dave Webb3
1

Lockheed Martin Advanced Technology Center, Palo Alto, CA, United States
The Aerospace Corporation, Los Angeles, CA, United States
3
Boston College, Boston, United States
2

nitta@lmsal.com

The Working Group 4 (Campaign Events) of the VarSITI/ISEST has identified a numberof Earth-affecting coronal mass ejections (CMEs) that present various challenges when we try tounderstand their origins on the Sun and effects at 1 AU. We discuss several examples from ourgrowing list of events, trying to clarify what we understand and what remain uncertain after ourrecent investigations. Our emphasis is on the origins of CMEs that were not accompanied byobvious low coronal signatures (LCSs). These CMEs characteristically start slowly. We showthat EUV images taken by the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics
Observatory (SDO) can reveal coronal dimming and a post-eruption arcade (compelling LCSs forCME), if we make difference images with long enough temporal separations that are commensuratewith the slow initial development of the CME. By providing the limb views of Earth-bound CMEs,
data from the EUV imager and COR coronagraphs of the Sun Earth Connection Coronal andHeliospheric Investigation (SECCHI) on the Solar Terrestrial Relations Observatory (STEREO) turnout to be very useful as they help us limit the time interval in which the CME forms and undergoes
initial acceleration. For other CMEs, we find similar but weaker LCSs, and only with lower
confidence. It is noted that even these less clear events may result in unambiguous flux rope
signatures in in situ data at 1 AU. There is a tendency that the CME source regions are located nearcoronal holes or open field regions. This may have implications for both the initiation of the stealthy
CME in the corona and its outcome in the heliosphere.
CHANGES IN OZONOSPHERE AND LOWER IONOSPHERE INDUCEDBY SOLAR PROTON EVENT OF 28 OCTOBER 2003 (3D SIMULATIONS)
Alexei Krivolutsky1, Lidiya Cherepanova1, Maik Wissing2
1
2

Central Aerological Observatory, Russia
University of Osnabruk, Osnabrück, Germany

krivolutsky@mail.ru

3D photochemical model CHARM-I (Chemical Atmospheric Research Model with Ions
[Krivolutsky et al., 2015] was used to study the response of neutral and ionized chemicalcompounds after Solar Proton Event of 28 October 2003. Model describes more than 200
reactions Ionization rates induced by particles has been calculated using AIMOS module[Wissing, Kalenrode, 2009] between the ground and 90 km. Ionization in both polar regions
generates additional neutral HOx and NOx and positive ions which disturbs neutral species (ogzone
and others), positive and negative ions, and electron density. Calculated ozone depletion looks
similar the corresponding effect obtained in HEPPA Project [Funke et al., 2011]. The result of
simulations showed that electron density was strongly increased after SPE over both regions.
103

IONOSPHERIC OBSERVATIONAL CAMPAIGN STUDY OF GEOSPACE STORMS:A SCENAIO FOR STRONG IONOSPHERE AND THERMOSPHERE COUPLING
DURING THE 2015 ST PATRICK’S DAY STORM
Shunrong Zhang
MIT Haystack Observatory99 Millstone RoadWestford, MA 01886USA, United States
shunrong@haystack.mit.edu

A number of ionospheric observational campaigns and analyses have been conductedduring the geospace storm events over the last a few years. The storm intensity spans different
levels and the storms have different solar and interplanetary drivers (i.e., CME and CIR types).
The most dramatic event was perhaps the 2015 St. Patricks Day that reached a minimum Dst at~ – 220 nT, the largest storm during the current solar cycle. We initiated the observations using a
network of incoherent scatter radars over America Sector, along with other more densely
distributed sensors (GPS receivers, FPIs, ionosondes, etc), to characterize ionosphere,
thermosphere, and magnetosphere responses. This presentation focuses on substantial I/T
perturbations caused by the presence of strong electrodynamic processes (e.g., subauroralpolarization stream, SAPS). These include strong ion-neutral frictional heating accompanied bylarge atmospheric upwelling, with ion upwelling as a potential source of ion upflow. Penetrationelectric fields were also measured by the Millstone Hill incoherent scatter radar during the storm
main phase and played important roles in creating the storm-enhanced density (SED) observed
during the event at subauroral latitudes extending into high latitudes. We will also discuss futureinternational observation campaign plans, in particular, along the meridian circle at

SUN-TO-EARTH PROPAGATION OF THE 2015 JUNE 21 CORONAL MASSEJECTION REVEALED BY OPTICAL, EUV, AND RADIO OBSERVATIONSNat Gopalswamy1, Pertti A Makela2, Sachiko Akiyama2, Seiji Yashiro2
1
2

NASA Goddard Space Flight Center, United States
The Catholic University of America, United States

nat.gopalswamy@nasa.gov

The 2015 June 21 double M flare was associated with a halo coronal mass ejection (CME)that resulted in all the familiar space weather effects: a large solar energetic particle event, aninterplanetary shock, and an intense geomagnetic storm. The geomagnetic storm was the second
largest in solar cycle 24 that resulted in significant ionospheric and radiation-belt changes. In thispaper, we consider the propagation of the CME-driven shock as revealed by the type II bursts at
metric and longer wavelengths. The eruption consisted of two M-class flares, with the first one
being marginally eruptive, with no metric or interplanetary radio bursts. However, there wasintense microwave burst, indicating accelerated particles injected toward the Sun. The second
flare was eruptive that resulted in a halo CME. The interplanetary type II burst was particularly
intense, and was visible all the way to the vicinity of the Wind spacecraft with fundamentalharmonic structure. The CME was fast (~1700 km/s), as expected because of its association witha large SEP event (>100 pfu in the >10 MeV channel) and a metric-to-kilometric type II radio
burst. The CME continued to accelerate in the coronagraph field of view, with interesting
consequences to the appearance of the type II burst in the interplanetary medium. Making use of104

the measured drift rate of the interplanetary type II burst, we were able to identify the
heliocentric distance where the CME/shock started deceleration. We also computed the shock
speed using the type II drift rates at various heliocentric distances and obtained information on
the evolution of the shock. Finally, we discuss the structure of the interplanetary CME that
resulted in the intense geomagnetic storm.
THE 2015 JUNE 22-23 STORM EFFECTS: FROM THE SUN TO THE EARTH
Yury Yasyukevich1, Vladimir Kalegaev2, Ilya Zhivetiev3, Natalya Kovyazina4,
Natalia Vlasova2
1

Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
Skobeltsyn Institute of Nuclear Physics, Lomonosov Moscow State University, Moscow, Russia
3
Institute of Cosmophysical Research and Radiowave Propagation FEB RAS, Paratunka, Russia
4
Irkutsk State University, Irkutsk, Russia
2

yasukevich@iszf.irk.ru

Our research is devoted to the 2015 June 22–23 magnetic storm. It was one on of the mostintense storms of the 24th solar cycle. We investigated whole chain of processes from the Sun to
the Earth. There were a lot of manifestations in different geophysical fields. The storm was
associated with coronal mass ejection (CME) linked with active region 2371. CME has speed of~1366 km/s and kinetic energy of ~ 9.0·1031 erg. When CME reached the Earth it compressed themagnetosphere and resulted in sudden storm commencement with positive H-SYM up to +88 nT.
Negative Bz component of interplanetary magnetic field produced strong magnetosphere
perturbation with intense variations in the Earth’s magnetic field. We also recorded sharp
decrease in H-SYM, increase in electrojet width and moving electrojet to lower latitudes, as well
as strengthened precipitation flux, pulsations, and magnetosphere convection. We revealed
strong displacement and intensification of equatorial anomaly crests, and sharp decrease inglobal electron content (up to 50 %). The storm resulted in strong large-scale ionosphereirregularities which originated at auroral oval boundaries and reached even opposite hemisphere.
Overall increase in total electron content slips was ~5–8 times against the quiet level. Variations
in solar wind parameters also influenced on observed galactic cosmic rays intensity. We also
recorded increase in solar proton flux at ~20 UT on June 22, which was found to be connectedwith M6.5 solar flare (June 22, start time 17:39; maximum 18:23) associated with the sameactive region 2371. The work is a result of activity during the COSPAR Capacity Building
Workshop. The study is partly supported by RF President Grant of Public Support for RF
Leading Scientific Schools (NSh-6894.2016.5) and by the RFBR project No. 15-05-03946.
RADIATION BELT RESPONSE TO THE MARCH 15, 2015 EVENT
Shrikanth Kanekal
NASA GSFC, United States
shrikanth.g.kanekal@nasa.gov

The geomagnetic storm of March 15, 2015 was the largest one observed during the past
decade. I will report on observations made by REPT (the Relativistic Electron and Proton
Telescope) and MagEIS (the Magnetic Electron and Ion Sensors) on board NASA’s Van Allen
Probes. Detailed spectral and pitch angle measurements covering electron energies from ~10’s of105

keV to ~10 MeV are obtained by MAgEIS and REPT. One of the pobes was serendipitously
located to observe the immediate electron response to the IP (interplanetary) shock that preceded
the CME driving the geomagnetic storm. The interplanetary shock that preceded the coronalmass ejection injected ultra-relativistic electrons almost instantaneously to L~3. Subsequently, over a
period of several days the radiation belts saw enhanced fluxes of very high energies of up to 8 MeV.

106

Session 6: ATMOSPHERIC RESPONSE TO SOLAR VARIABILITY
AND MODULATION OF ITS IMPACT ON TIMESCALESFROM MINUTES TO DECADES__________________________________________________________________ATMOSPHERIC IMPACTS OF THE STRONGEST KNOWNSOLAR PARTICLE STORM OF 775 AD
Timofei Sukhodolov
Physikalisch-Meteorologisches Observatorium Davos World Radiation Centre, Davos, Switzerland
timofei.sukhodolov@pmodwrc.ch

A severe solar energetic particle storm, which took place in 774–775 AD, was the greatest
one over 11 millennia, 40–50 times stronger than the largest event directly recorded during themodern instrumental era. This offers a unique opportunity to test the existing models and assessa potential impact on the Earth’s atmosphere for a realistic worst case scenario. Here we presenta systematic analysis of this severe event using the available data and up-to-date models. First
we reproduce, with the atmospheric climate chemistry model SOCOL and the 10Be production
model CRAC, the observed variability of cosmogenic isotope 10Be in four different ice coresfrom Greenland and Antarctica, thus confirming the validity of the models and the input energy
spectrum. Furthermore, important for determining the correct dynamical consequences, themodel results suggest that the event likely occurred during boreal autumn. Next, we calculated
the amount of nitrate deposited in different polar ice cores and compare those with theobservations. We show that, contrary to some earlier claims, even such an extreme solar particle
storm cannot produce a notable peak in nitrate concentration. Finally, we assess the possible
effect of this uniquely strong event on the Earth’s atmosphere and found statistically significant
negative total ozone changes lasting for at least one and a half years after the event and changesof the surface weather in the northern hemisphere during the winter after the event.
PROPAGATION OF STATIONARY PLANETARY WAVES FROM THE LOWER
TO THE UPPER ATMOSPHERE AT DIFFERENT LEVELS OF SOLAR ACTIVITY
Nikolai Gavrilov1, Andrej Koval1, Alexander Pogoreltsev2, Nikita Shevchuk1
1
2Saint Petersburg State University, Saint Petersburg, Russia
Russian State Hydrometeorological University, Saint Petersburg, Russia

n.gavrilov@spbu.ru

Changes of zonal circulation and amplitudes of stationary planetary waves (SPWs) in theatmosphere at different levels of solar activity (SA) are studied. General circulation model of the
middle and upper atmosphere MUAM is used. To account for changes in solar activity in themodel a set of different values of solar radio emission flux at wavelength of 10.7 cm is used.
Ionospheric conductivities are also taken into account with their latitudinal, longitudinal and timedependencies calculated for different SA levels. The simulation includes general atmosphericcirculation, amplitudes of SPWs with zonal wave numbers 1 and 2, refractive indices for SPWs
and Eliassen-Palm fluxes corresponding to considered SPWs. Simulations are carried out for
January-February and conditions of low, medium and high solar activity. It is shown that at highSA the zonal winds are larger at altitudes above 150 km and smaller at lower altitudes. At high
SA SPW amplitudes are smaller at altitudes above 120 km and are larger at altitudes lower than
100 km, than those at low SA. These differences correspond to the calculated changes in the107

SPW refractive index of the atmosphere and Eliassen-Palm flux. Changes in conditions of SPW
propagation in the thermosphere at different levels of solar activity may affect changes in SPW
amplitudes and atmospheric circulation at smaller heights in the middle atmosphere.
USING THE EMISSIONS OF EXCITED OXYGEN TO STUDY FAST [O3]VARIATIONS IN THE MESOSPHERE AND LOWER THERMOSPHERE
Rada Manuilova, Valentine Yankovsky
Atmospheric Physics Department, Saint Petersburg State University, Saint Petersburg, Russia
nansey@yandex.ru

In the framework of the model of electronic vibrational kinetics of excited products of O3
and O2 photolysis in the MLT of the Earth, YM2011, we study the possibilities of retrieval the[O3] altitude profiles using as proxies electronic-vibrationally excited levels of oxygen molecule,namely O₂(b1, v=0, 1), O₂(a1, v=0) and excited atom O(1D). Population of O2 (b1, v=2)
doesn’t depend on [O3]. Concerning the [O3] retrieval in the range of 50–100 km, the emission
at 1.27 μm formed by transition from O₂(a1, v=0) and emission at 762 nm formed by transition
from O₂(b1, v=0) are the most intensive ones among all emissions under consideration. However,considering the complexity of kinetics of the excited components: choosing O₂(a1, v=0) as aproxy for [O3] retrieval requires taking into account 25 aeronomical reactions. For other proxies
the number of aeronomical reactions is as follows: O₂(b1, v=0)−18; O₂(b1, v=1)−13; O₂(1D,v=0)−5. Increasing the number of reactions that must be considered when using a proxy from
O(1D) to O₂(a1, v=0) depends on the fact that, calculating the population of each of theunderlying electronic-vibrationally excited state requires considering the mechanisms of the
population of the upper levels. Therefore, O₂(b1, v=1) is the preferable proxy at the altitudes of50−98 km. Commonly used [O3] retrieval proxy, O₂(a1, v=0), transition from which forms the
1.27 μm O2 IR Atmospheric band, has more than one hour photochemical lifetime in the MLT
region. On the other hand, the O(1D) and O₂(b1, v=0, 1) lifetime in the altitude region of 50−120 km
is less than 14 sec. So, the proposed O₂(b1, v=0, 1) and O(1D) proxies can be used for tracking fastvariations of the O3 atmospheric concentrations generated by wave processes, electron precipitations,
solar flux changes, and so on, when the O₂(a1, v=0) proxy becomes useless.
INFLUENCE OF SOLAR ACTIVITY ON INDIAN SUMMERMONSOON RAINFALL FOR THE LAST FIVE CENTURIES
Sourabh Bal
Swami Vivekananda Institute of Science and Technology, Kolkata, India
sourabhbal@gmail.com

Previous studies investigating the relationship between solar activity and Indian Summer
Monsoon Rainfall (ISMR) using instrumental records have been reported. Temporal scale ofobserved Sunspot numbers (since 1700) and recorded ISMR time series (starts from 1871) are aconstraint to study any relation between solar cycle and ISMR in the multi-decadal variability scale.
So, this present research effort investigates decadal and multi-decadal variability in the ISMR and its
teleconnection with solar activity using proxy reconstructions for few centuries before present.
Increased precipitation in the tropical region favors growth of tree rings. Speleotherm records canalso yield similar rainfall estimates like tree rings. Both tree rings and speleotherm records is used as
ISMR proxy data. Simulated Sunspot numbers are available to study its teleconnection with ISMR
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for the last 500 years. Correlation between ISMR and solar cycle is not very pronounced for theconsidered time span but improves significantly in discontinues temporal scale. Wavelet analysis andcross-wavelet transform are also employed to study the time series of ISMR and Sunspot numbers.
The recognized 11-year solar cycle are determined in the ISMR time series. The periods of 2–5 years
are found to exist in the summer monsoon rainfall over India.
SOLAR EFFECTS ON THE UPPER ATMOSPHERE FROM SOLAR FLARETO SOLAR CYCLE TIME SCALES
Liying Qian
National Center for Atmospheric Research, Boulder, United Stateslqian@ucar.edu

Solar irradiance is the primary energy input to the thermosphere/ionosphere system. The
thermosphere absorbs solar irradiance in XUV (the soft X-ray ultra-violet, 1–30 nm), EUV (extreme
ultra-violet, 30–120 nm), and FUV (far ultra-violet, 120–200 nm). The solar EUV ionizes,
dissociates, and excites the thermospheric constituents, creates the ionosphere, and heats thethermosphere. In this presentation, we discuss solar irradiance variations from solar flare to solar
cycle time scales, and their effects on the upper atmosphere, from the perspective of modeling anddata results of thermosphere neutral density due to these variations in solar irradiance. We will
discuss variations in neutral density include abrupt changes with a time scale of minutes to hours due
to solar flare, diurnal variation, solar-rotational variation, annual/semiannual variation, and solarcycle variation. The neutral density data sets include neutral density observed by the accelerometers
onboard the Challenging Mini-satellite Payload (CHAMP), neutral density at satellite perigees, andglobal-mean neutral density derived from thousands of orbiting objects. Modeling results are fromthe National Center for Atmospheric Research (NCAR) thermosphere-ionosphere-electrodynamics
general circulation model (TIE-GCM), and from the NRLMSISE-00 empirical model.
SOLAR AND GEOMAGNETIC CONTROL OF IONOSPHERIC WINTER ANOMALYAND SUMMER EVENING ANOMALY IN NMF2 AND TEC
Maxim Klimenko1,2, Konstantin Ratovsky3, Vladimir Klimenko1,
Yury Yasyukevich3, Anna Yasyukevich3, Nikolay Chirik1, Alexander Markov2,
Alisher Abdullaev2, Nina Korenkova1
1

West Department of Pushkov Institute of Terrestrial Magnetism, Ionosphere and Radio Wave
Propagation RAS, Kaliningrad, Russia
2
Immanuel Kant Baltic Federal University, Kaliningrad, Russia
3
Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
maksim.klimenko@mail.ru

We analyzed the winter anomaly (WA) and mid-latitude summer evening anomaly (MSEA)
manifestation in the F2 peak electron density (NmF2) and Total Electron Content (TEC) based on theobservation data and model calculation results. For the analysis we used 1998–2015 TEC Global
Ionospheric Maps (GIM), NmF2 ground-based ionosonde observation data and COSMIC, CHAMP
and GRACE radio occultation ionospheric data. We also used the Global Self-consistent Model of
the Thermosphere, Ionosphere, and Protonosphere (GSM TIP) and the International Reference
Ionosphere model (IRI-2012). Based on the observation data and model calculation results weconstructed the maps of the WA and MSEA intensity in TEC and NmF2 for the different levels of109solar and geomagnetic activity. According to both observation and modeling we found that the
winter anomaly intensity was higher:
1) in NmF2 than in TEC;
2) during solar maximum than in solar minimum;3) for the greater level of geomagnetic activity.
MSEA appears earlier in TEC than in NmF2. The MSEA intensity does not depend on the levelof geomagnetic activity. We investigate in detail the formation mechanisms of longitudinalvariability and interhemispheric differences in WA and MSEA. It is shown that the vertical plasmatransport along geomagnetic field lines due to the thermospheric wind at heights of ionosphere F
region plays an important role in the formation of longitudinal variability in WA and MSEA. The
possible reasons of MSEA and WA interhemispheric asymmetry are also discussed.
NONLINEAR SPECTRAL ANALYSIS OF CARBON C14
FOR THE LAST 12.000 YEARS: ABRUPT CLIMATE CHANGESIN THE PAST AND FUTURE
Tamara Kuznetsova
Pushkov Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation RAS,
Moscow, Russia
tvkuz3@gmail.com

The important evidence within the last years has accumulated the capacity of the climate
system to undergo major changes on time scales of less than a century, in some cases, less thandecade. Abrupt climate fluctuations at period T~1500 yr were revealed during the last glacial
period in the Greenland ice cores. Similar fluctuations during Holocene are referred to Bond
events (BEs), but their connection with climate is poorly studied. Bond et al (1997) identified 8
events based on tracers of drift ice. Causes of the BEs are unknown, main focus to solar activity
and atmosphere circulation. Because the BEs points to nonlinearity and resonance a non-linear
spectral analysis has to be used. We use the MGM method elaborated by us, which is capable ofmaking a self-consistent selection of trends from a data set and singling out harmonics withvarying phase and amplitude. C14 is produced in the troposphere and stratosphere. Source isgalactic cosmic ray flux, which is controlled mainly by solar activity and geomagnetic field. We use
a set of C14 (9700 yr BC – 1980 yr AD). Main aim is to analyze the most power nonstationary
and long-term components for the results to compare with the BEs and temperature (GIPS cores).
The trend described by sinusoid at T=18.6 kyr has the highest amplitude and can be interpreted
as a term in climate precession of Milankovich. The trend is coming to the C14 absolute
minimum for now. A nonstationary sinusoid at T=2600 yr shows intervals of damping andbuilding-up oscillations (decrease and increase of amplitude). The amplitude began to rise
rapidly long before AD era (a manmade cause is eliminated) and increased the value at the endof BC era by twice at present. The cycle is coming to absolute minimum in C14 (warming).
Nearness of the minimum to the trend minimum points to reorganization of geophysical systems
in the future. The power nonstationary sinusoid at T=2230 yr also shows intervals of damping
and building-up oscillations. The amplitude also began to rise during years BC, but one has not
yet reached maximal values. We show how variations of the 2230-yr and 2600-yr sinusoids
create recurrent T~1500 yr of the abrupt changes (BEs). We discuss connection of the spectral
periods with periods of astronomical origin and possible physical mechanisms. Finally we
propose expected evolution of climate in the near future.

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WAVE AMPLIFICATION DURING SOLAR EVENTS BASEDON THE OBSERVATIONS OF ELECTRIC PARAMETERS
OF THE NEAR GROUND ATMOSPHERE
Sergey Smirnov
Institute of Cosmophysical Research and Radio Wave Propagation FEB RAS, Paratunka, Russia
sergey@ikir.ru

Spectral analysis of meteorological (air temperature, humidity, pressure) and of electric
quantities (quasi-static electric field strength and air electrical conductivity) in the near groundatmosphere has been carried out. In the presence of the prevailing component with the period of
24 hours, an additional component with the period of 48 hours appeared in the power spectra of
meteorological quantities during solar events in “fair weather” conditions. In the power spectraof atmospheric electric conductivity and electric field strength, the components of both thermal
tidal and planetary waves were observed with the development of solar and geomagnetic activity.
Intensities of the components with the periods of planetary waves increased by an order. In the
power spectra of galactic cosmic ray fluxes accompanying strong solar flares, the components
with the period of 48 hours prevailed with the appearance of additional components of weakerintensity with the period of 24 hours. Simultaneous intensification of the components with theperiod of 48 hours in the power spectra of electric conductivity and electric field strength
indicate the fact that during strong solar flares and geomagnetic storms, mainly the galactic
cosmic rays are the acting ionizers of the lower troposphere.

DIFFERENCES IN THE INTENSITY OF THE STRATOSPHERIC
CIRCULATION MERIDIONALITY FOR THE SOLAR MAXIMAAND MINIMA CONDITIONSElena Devyatova1, Vladimir Mordvinov1,
Pavel Antokhin2, Olga Antokhina2
12Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
V.E. Zuev Institute of Atmospheric Optics SB RAS, Tomsk, Russia

devyatova@iszf.irk.ru

Differences in the intensity of the stratospheric circulation meridionality for the solar maxima
and minima conditions were investigated using NCEP/NCAR Reanalysis and ECMWF ERA-Interim
1968–2010. We found that in the stratosphere of both hemispheres meridionality index in the solar
maxima periods is lower than in the solar minima periods for all seasons except summer in the
Northern Hemisphere (June–August) and autumn in the Southern Hemisphere (March, April).

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LONG-TERM VARIABILITY AND TREND OF THE MESOSPHERE BASEDON PHASE-HEIGHT MEASUREMENTS OVER EUROPE
Dieter H.W. Peters, Günter Entzian, Dieter Keuer, Jorge L. Chau
Leibniz-IAP, University of Rostock, Kühlungsborn, Mecklenburg, Germany
peters@iap-kborn.de

Phase-height measurements of low frequency radio waves are used to study the long-term
variability and trend of the mesosphere (D layer, about 80 km altitude) over Europe. The conceptof standard phase heights (SPH) warrants the continuity of the series in the case of slightfrequency changes. The advantages of the method are the low costs and the simplicity ofoperation. The signal was received at Kühlungsborn (54° N, 12° E, Mecklenburg, Northern
Germany). Since February 1959, that means over more than 5 solar cycles, field strength
measurements of the broadcasting station, Allouis (Central France), have been maintained andreanalyzed. The mean annual cycle of SPH-series shows a negative winter anomaly known to be
due to enhanced downward transport of NO and subsequent photo-ionization. Stratosphericinfluences of QBO-like and ENSO-like oscillations on mesospheric SPHs have been shown forsolar minimum phases. The SPH-series are partially anti-correlated to the solar cycle because
stronger photo-ionization is linked with higher number of electrons, which reduces the SPH.
Furthermore the statistical analysis of the SPH-series shows a significant overall trend in theorder of hundred meters per decade induced by a shrinking stratosphere due to global warming
but with strong intra-decadal variability in winter. In order to exclude the influence of the winteranomaly in the determination of column-integrated mesospheric temperature trends, ourprocedure is confined to summer months. The derived thickness temperature of the mesospheredecreased statistically significant over the period 1959–2008 after pre-whitening with summer
mean of solar sun spot numbers. The trend value is in the order of about –1.05 K/ decade if thestratopause trend is excluded. The linear regression is stronger, –1.35 K/ decade for the period of
1963–1985 (2 SCs), but weaker, –0.51 K/ decade during 1986–1908 (last 2 SCs).
THE ENERGY BUDGET OF THE MESOSPHERE
AND THERMOSPHERE — RESULTS FROM 15 YEARS OF SABER,SORCE, AND SEE OBSERVATIONSMartin Mlynczak1, Linda Hunt2, B. Thomas Marshall3, James Russell III4
1

Climate Science Branch NASA Langley Research Center, United States
Science Systems Applications Incorporated, Hampton, United States
3
Global Atmospheric Technologies and Sciences (GATS), United States
4
Hampton University, Hampton, United States2

m.g.mlynczak@nasa.gov

The energy budget of the mesosphere and thermosphere (MLT) is exceptionally complex.
Energy in the form of ultraviolet radiation is deposited from the Sun, setting off a chain ofphotochemical processes leading to the generation of heat and airglow in the region. Collisionaland radiative processes internal to the MLT result in the lowering of the kinetic temperature
through loss of energy by infrared radiation. All of these heating and cooling processes occur far
from local thermodynamic equilibrium, and are said to be in “non-LTE.” The SABER instrument,
now in its 16th year of operations on the NASA TIMED satellite, was designed to provide
measurements from which nearly all of the individual processes contributing to the energy
budget of the MLT could be derived. These processes include the absorption of solar radiation
by molecular oxygen and ozone from Ly-α to visible to near-infrared wavelengths; seven112

exothermic chemical reactions; and infrared radiative cooling. In this talk we will present the
MLT energy budget as derived from SABER observations with solar irradiances provided by theSEE instrument on TIMED and instruments on the SORCE satellite. Approximate balance
between heating and cooling is found in annual timescales. There is a clear solar cycle
dependence evident in all terms of the energy budget and in the total heating and total coolingterms. Energy balance also provides a critical test for some SABER data products such as atomic
oxygen, and these will be reviewed in detail. The talk will conclude with a look to the future on
concepts to continue these observations after the end of the TIMED epoch.
CLIMATE VARIATIONS INITIATED BY JOINT EFFECTOF SOLAR UV VARIABILITY AND THE ACTIVITY
OF PLANETARY WAVES (SIMULATIONS WITH ARM AND DATA ANALYSIS
Alexei Krivolutsky, Alla Dementeva, Lidiya Cherepanova
Central Aerological Observatory, Moscow, Russia
krivolutsky@mail.ru

GCM ARM (Atmospheric Research Model [Krivolutsky et al., 2015] was used to simulate
global response of atmospheric temperature and wind to variability in solar UV radiation. Upper
boundary of ARM is at 135 km. Global fields of radiative-active gases were incorporated from
3D global photochemical model CHARM [Krivolutsky et al., 2015]. Planetary waves structure in
the model. The results of simulations showed that temperature response has wave-like structurewith its amplitudes which are more than several K. So, revealed response has several minima andmaxima along the latitude. Using reanalysis data the similar wave-like restructure was found.
INFLUENCES OF CLIMATE FORCING FACTORS ON TEMPERATURE
ANOMALIES AT REGIONAL SCALES
Rolf Heinz Werner1, Dimitar Valev1, Dimitar Danov2, Veneta Guineva1,
Andrey Kirillov3
1

Space Research and Technology Institute, Bulgarian Academy of Sciences, Stara Zagora
Department, Stara Zagora, Bulgaria
2
Space Research and Technology Institute, Bulgarian Academy of Sciences, Sofia, Bulgaria
3
Polar Geophysical Institute of the Kola Science Centre RAS, Apatity, Russia
rolwer52@yahoo.co.uk

Statistical regression models describing temperature anomalies change include several
climate factors. Usually external factors as atmospheric CO2 content, volcanic emissions, andthe total solar irradiation and some internal factors as teleconnections are included in the models.
The factors are taken into account directly or as indices in a linear regression model. If themodels are used to describe global or hemispheric temperature anomalies the number of internal
factors is reduced. Depending on the used temperature data sets and whether temperature
anomalies over land or sea are modelled, only one or two internal factors, namely the El NiñoSouthern oscillation or the stratospheric aerosols loaded by volcano eruptions have a significant
climate impact. In the case of the estimation of the temperature anomalies at regional scales in
the model predictors describing the Pacific decadal oscillation and the North Atlantic oscillation
have to be included. As it is well known they have an important influence on the temperature andon other climate parameters at large regional scales and generate weather phenomena. Globally,
the influence of the solar irradiation on the climate is small and in general is less than 0.1 °C, but
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it becomes larger at regional scales. Based on the HadCRUT version 4.4.0.0 gridded annual
temperature data set we have constructed global maps presenting the influence of different
climate factors on the temperature and maps showing their estimated significances for the time
period from 1900 to 2015. In addition to the mentioned above factors contributing to temperaturechanges we studied also the influence of the Atlantic multidecadal oscillation. The maps wereconstructed by estimation of the temperature impacts of all factors simultaneously in all 5 deg. x
5 deg. grid points by solving the multiple linear regression equation. Besides we present maps
for the warming and cooling phase of the climate factors. The results are briefly discussed.
LONG-TERM GLOBAL TEMPERATURE VARIATIONS UNDER TOTAL SOLAR
IRRADIANCE, COSMIC RAYS, AND VOLCANIC ACTIVITY
Lilia Biktash
Pushkov Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation RAS,
Moscow, Russia
lilia_biktash@mail.ru

The effects of total solar irradiance (TSI), cosmic rays, and volcanic activity on long-term
global surface air temperature variations (GSAT) during solar cycles 19–24 was studied. It was
shown that a large proportion of climate variations can be explained by the mechanism of actionof TSI and cosmic rays (CRs) on the state of the lower atmosphere and other meteorologicalparameters. The trends of sunspot numbers, CRs, and IMF B (module of interplanetary magnetic
field) for 20–24 solar cycles do not show a significant effect, whilst the global temperatures(GSAT) trend is very large, and significant. This is a forcible argument to attribute GSAT trend
to human activity. The role of volcanic signals in the 11-year variations of the Earth’s climate
can be expressed as several years of global temperature drop. Conversely, it was shown that theeffects of solar, geophysical, and human activity on climate change interact. It was concluded
that more detailed investigations of these very complicated relationships are required, in order tobe able to understand issues that affect ecosystems on a global scale.
THERMOSPHERIC RESPONSE TO SOLAR VARIABILITYFROM MORE THAN 15 YEARS OF SABER DATA
Linda Allen Hunt1, Martin Mlynczak2, Bruce Tsurutani3,
Jesper Gjerloev4, James Russell5
1

Science Systems and Applications, Inc. at NASA Langley Research Center, United States
NASA Langley Research Center, United States
3
NASA Jet Propulsion Laboratory, Pasadena, CA, United States
4
Johns Hopkins University, Laurel, MD, United States
5
Hampton University, Hampton, VA, United States
2

Linda.A.Hunt@nasa.gov

Infrared radiation, from nitric oxide (NO) at 5.3 μm and carbon dioxide (CO2) at 15 μm, isthe dominant mechanism by which the thermosphere cools to space. The Sounding of the
Atmosphere using Broadband Emission Radiometry (SABER) instrument on the NASA
Thermosphere Ionosphere Mesosphere Energetics and Dynamics (TIMED) satellite has beenmeasuring thermospheric cooling by NO and CO2 since January, 2002. Physically, changes in114

NO emission are due to changes in temperature, atomic oxygen, and the NO density, while for
CO2, the emission change is most directly related to temperature and atomic oxygen. Thesephysical changes are driven by changes in solar irradiance and geomagnetic conditions. We see
evidence of these changes on timescales from minutes to days, over a single solar cycle and,through reconstruction using multiple linear regression fits, over multiple solar cycles. As thecoronal structure of the sun changes over a solar cycle, new periodicities are seen in the data set.
And in our most recent analysis of solar storm impacts, we find infrared cooling effects at the
sub-storm level, on the order of minutes. These findings provide valuable insight into the global
infrared energy budget and chemistry of the thermosphere over a variety of time periods.
ON THE MECHANISM OF INFLUENCE OF HELIOGEOPHYSICALDISTURBANCES ON THE EARTH TROPOSPHERE
Sergey Molodykh
Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
sim@iszf.irk.ru

Observational data of characteristics of heliogeophysical disturbances influencing on Earth,and data of the troposphere properties are analyzed. Taking into account an open character ofclimate system through which a considerable energy flux from the Sun passes, and insignificant
external actions on climate system, a considerable response is shown to be only if there is an
influence on the climate system parameters, which control solar energy passing through theclimate system. As shown from the analysis the most effective mechanism of an influence on anenergy flux passing is that modulates optical properties of the atmosphere in long-wave(infrared) spectral range. The features of the mechanism, developed in ISTP are discussed indetail. It is noted that the analysis of observations carried out during of the heliogeophysicaldisturbances does not reveal data disagreed with that. The mechanism allows us to explain somepeculiarities of the troposphere response to heliogeophysical disturbances. The peculiarities are
spatial inhomogeneity and ambiguity of the response, as well as variability of its spatial structure.
The time lag of the troposphere temperature response to separate heliogeophysical events of lessthan one hour duration is estimated.
LONG-TERM SPECTRAL COMPONENTS OF GLOBALAND HEMISPHERE TEMPERATURES OVER THE LAST MILLENNIUM
AND SOLAR FORCING
Tamara Kuznetsova
Pushkov Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation RAS,
Moscow, Russia
tvkuz3@gmail.com

Variations of solar radiation reaching the Earth have two main causes. The first is relatedwith the 11-yr solar cycle: at the maximum the total solar irradiance was larger by 0.1 % than at
the minimum, which could cause surface temperature changes of a few tenths of degree ofCelsius. Recent oppositely directed trends in solar climate forcing and global mean surface airtemperature shows that recent rise in the temperature cannot be attributed to solar effects. The
second cause is related with solar radiation (insolation) reaching the Earth due to varying
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distance from Sun. Milankovich theorized that three geometric relations between Earth and Sun(eccentricity, axial tilt and longitude of perihelion) resulted in cyclical variation of solar radiation(insolation) reaching the Earth and influenced on climate. Astronomers estimate that in 1246 theDecember solstice was on the same day as the Earth reached its perihelion. One of the aims of
the study was to detect response of trends in the Global, North and South hemispheretemperatures (Tgl, Tnh and Tsh) to the Earth’s transition the special year. The problems are trends,
quasi-periodicities and noise in climate processes. We use the Method of Global Minimum
elaborated by us, which is capable of making a self-consistent selection of trends from a data set
and singling out harmonics with varying phase and amplitude. Annual anomalies in temperaturefrom 17 sites worldwide for the last 1000 yr and annual sunspot numbers W for the last 205-yr
are used. Trend in Tnh described by nonstationary sinusoid at period T=1270 yr shows maximum
near 1300 (medieval time), minimum at 1700 (Maunder) and rise since 1700. We obtained theperiod in spectrum of carbon C14 for the last 12.000 yr and showed its relation with climate andaxial precession. Trend in Tgl described by nonstationary sinusoid at T=1000 yr shows warming
near 1350, deep cooling at 1750 and stable warming after 1750. We also obtained the period inspectrum of C14 and showed its connection with climate and precession of perihelion. The results
lead to expected maximum of Tgl near 2250. We demonstrate parameters of the 1000-yr cycle: its
amplitude decrease before 1250 (damping of oscillations) and the amplitude increase withconstant velocity after the year (building-up of oscillations). The amplitude for present in thedata is six times the amplitude in 1250 and one is 3.7 times larger than the amplitude of the 200yr cycle in Tgl, which varies in phase with the 200-yr cycle in W. Finally we present results of
our analysis of common periods from spectra of Tgl and W for influence of the sunspot activity
on climate to understand.
PECULIARITIES OF THE GEOMAGNETIC FIELD VARIATIONSIN QUIET AND DISTURBED CONDITIONS
Boris Shpynev, Denis Khabituev
Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
shpynev@iszf.irk.ru

In the present study we consider different aspects of the geomagnetic field activity on thebase of global indexes and magnetometers data for Northern hemisphere. From the analysis of
Kp–Ap indices it has been found that in quiet geomagnetic conditions the significant part of dayto-day geomagnetic field variations are caused by gravity field variations due to lunar-solar tidal
forcing. This produces the geomagnetic field variations with periods 9.1, 13.66 and 27.55 days
that are especially strong during the low solar activity periods. The longitudinal structure of thegeomagnetic field variations is studied on the base of two magnetometer chains in the Northernhemisphere each consisted of 12 magnetometers located near latitudes ~55° N and 70° N. It has
been found that the geomagnetic field variability has irregular longitudinal structure due todifference of geographic and geomagnetic poles. During the low geomagnetic activity ingeographic coordinates the zone of high geomagnetic field variations is obviously shifted toward
the magnetic pole meridian ~270°. However, during the magnetically disturbed periods two
active zones form symmetrically opposite to the geomagnetic pole at ~40° and ~130° longitudes.
Between these two zones a sector with lowest geomagnetic field variations always forms atlongitudes 80–110°.

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CONTRIBUTION OF RELATIVISTIC ELECTRON PRECIPITATIONFROM RADIATION BELT TO THE TOTAL OZONE CONTENTOVER HIGH LATITUDES AND ENTIRE GLOBE
Arseniy Karagodin, Irina Mironova
Saint Petersburg State University, Saint Petersburg, Russia
karars94@mail.ru

In this work we investigated a response of the total ozone column on precipitations ofrelativistic electrons from the radiation belts. Here we used the method of superposed epoch
analysis and as key dates were chosen the events of relativistic electron precipitation from 1961
to 2014. The list of events was prepared by members of the balloon experiments of the Lebedev
Physical Institute of RAS. For our study, we selected the events registered during the winter(from November to February) and summer months (from June to August) since 1970 to 2012.
These years were chosen, based on the data of the total ozone column obtained during themeasurements SCIAMACHY, OMI, GOME. A long series of measurements of the total ozone
column allowed studying 90 winter and 101 summer events of relativistic electron precipitation.
The results of superposed epoch analysis show that total ozone column responds to relativistic
electron precipitations. In the polar region the total ozone content is reduced after relativistic
electron precipitation (in winter time) and the minimum is observed on the first day after the
event. The obtained ozone sensitivity to summer and winter REP events is more clear
pronounced in the middle and higher latitudes of the Northern Hemisphere, with the latitudinalmaxima about 50 NH.

RADIOCARBON EVIDENCE OF SEASONAL ATMOSPHERE—OCEANGAS EXCHANGE
Alexey Byalko
Landau Institute for Theoretical Physics, Chernogolovka, Russia
alexey@byalko.ru

In nuclear explosions in the atmosphere neutrons react with air nitrogen forming
radiocarbon. As a result, by October 1965 when the international treaty banning nuclear tests inthe atmosphere came into force the content of radiocarbon in the atmosphere exceeded its levelof 1950 more than twice. However, then measurements of its concentration showed an
exponentially fast decrease. In the atmosphere radiocarbon is present in the form of 14CO2. Itsabsorption by water, as well as all chemical reactions of radiocarbon and stable carbon isotopes are
identical. A joint study of regular trends in concentrations of 14C and CO2 as well as their seasonalvariations provides unique information on gas exchange between the atmosphere and the ocean.

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DYNAMICAL PERTURBATIONS OF THE THERMOSPHERE
IN THE SOUTHERN HEMISPHERE INFERREDFROM SATELLITE OBSERVATIONS OF O(1D) NIGHTGLOW AND TECMarianna Genova Shepherd1, Gordon Shepherd1, Young-Min Cho1, Mihail Codrescu2
1

Centre for Research in Earth and Space Science, York University, Toronto, Canada
Space Weather Prediction Center, National Centers for Environmental Prediction, Boulder,
United States2

mshepher@yorku.ca

The Midnight Temperature Maximum (MTM) is a large scale neutral temperature anomaly
with a wide-ranging effect on the nighttime thermospheric dynamics at low latitudes. The focusof the current study is an investigation of the extent of the MTM to southern low and midlatitudes (5–40° S) employing multi-year observations of O(1D) airglow volume emission rates(VER), Doppler temperatures (DoT), and neutral winds over the altitude range of 190–300 km by
the Wind Imaging Interferometer (WINDII) experiment on board the Upper Atmosphere
Research Satellite. The MTM dependence on longitude, season, local time and altitude has been
examined. The observed perturbations in the O(1D) VER and temperature were out-of-phase withrespect to longitude. Latitude/longitude maps of the VER and DoT revealed wave-1 and wave-3
signatures most persistently seen after local midnight in summer, with very little day-to-day
variation in phase, while the amplitude varied with time. WINDII meridional wind observations, aswell as correlative in time TOPEX TEC (Total Electron Content) data have been employed toinvestigate the mechanisms underlying the observed enhancement in O(1D) VER and DoT,
including the possible relationship to the Weddell Sea Anomaly in the observed perturbations.

UPPER ATMOSPHERE CONDUCTIVITY MODEL AND CONDUCTIVITIESEFFECTS ON MODELING OF ATMOSPHERIC TIDES AT DIFFERENT LEVELSOF SOLAR ACTIVITY
Nikita ShevchukDepartment of Atmospheric Physics, St. Petersburg University, St. Petersburg-Petrodvorets, Russia
n.o.shevchuk@mail.ru

Middle and Upper Atmosphere Model (MUAM) is used for numerical simulation of
atmospheric tides amplitudes changes due to effect of different levels of solar activity. The levelof solar activity (SA) is specified using different radio flux values of the sun radiation withwavelength 10.7 cm. Ionospheric conductivity model developed allows to take into accountlatitudinal, longitudinal, and temporal conductivity variations at the different solar activity levels.
The calculations are performed for January-February and the low, medium and high SA. The
analysis of the effect exerted by different levels of solar activity in migrating and non-migratingtides latitude-height structure is performed.

118

EMPIRICAL MODEL OF SPATIAL-TEMPORAL VARIATIONSIN THE INTENSITY OF CARBON DIOXIDE (15 MICRONS) INFRARED RADIATION
IN THE UPPER ATMOSPHERE
Anatoly Semenov1, Irina Medvedeva2, Vladimir Perminov1, Vladislav Khomich3
1

Obukhov Institute of Atmospheric Physics RAS, Moscow, Russia
Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
3
Institute of Problems of Electrophysics RAS, St. Petersburg, Russia
2

ivmed@iszf.irk.ru

We present the results of systematization and analysis of long-term data from rocket andsatellite measurements of the carbon dioxide CO2 (15 microns) infrared (IR) radiation in theupper atmosphere. This radiation originating at the upper mesosphere and lower thermosphere(MLT) heights plays a very important role in forming the thermal regime of the upper
atmosphere and energy balance at these altitudes. The importance of studying the IR spatialtemporal variations is caused by the necessity to take into account the peculiarities of regionalvariations in the upper atmosphere temperature regime in predictive estimations of the global
pattern of the upper atmosphere cooling processes at different latitudes over different timeintervals during a year (diurnal and seasonal variations, etc). Photochemical atmosphericprocesses, leading to the origin of the 15 microns CO2 emission, were analyzed. Based on thestatistical analysis of the published data from rocket and satellite measurements of carbon
dioxide IR radiation in the upper atmosphere over recent 30 years, we obtained analyticalequations (empirical model). The model describes height distribution of the 15 microns emission
intensity, its seasonal and latitudinal variations, and its dependence on solar activity. The CO2
emission intensity behavior dependence on the solar activity is shown to have a nonlinear
character. Analysis of seasonal variations in CO2 emission intensity revealed its minimum insummer and maximum in winter. Latitudinal behavior of CO2 emission intensity was studied.
Analyzing the dependence of the annual mean CO2 emission intensity on the geographicallatitude revealed that the intensity increases in both hemispheres as the latitude increases. In theequatorial region, there is a small maximum in the CO2 emission intensity. This study was
supported by the Russian Foundation for Basic Research (Project No. 16-05-00120-a).
SOLAR ACTIVITY VARIATIONS INDUCING EFFECTS OF LIGHT SCATERRING
AND REFRACTION IN THE EARTH`S ATMOSPHERE
Pavel Kovadlo1, Vladimir Lukin1, Artem Shikhovtsev1, Elena Kochugova2
1
2

Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
Irkutsk State University, Irkutsk, Russia

kovadlo2006@rambler.ru

Possible mechanism of solar activity effect on scattered radiation as well as the intensity of
exchange processes in the earths troposphere is discussed in this paper. In particular, theresponse of the Earth’s atmosphere optical characteristics to the 11 year variations of the sunspot
formation activity is considered. Analysis of the radiation data show that significant growth ofthe mean annual values of scattered radiation is observed while a total solar activity decreasing
in certain years. This earth`s atmospheric characteristic is related to the quality of images ofspace objects — called seeing in astronomical practice. The effect of solar activity on the
scattered radiation fluctuations is most pronounced over a long time periods, the duration ofwhich is more than 11 years. The effect of any connection becomes invisible at short timeintervals, when high-frequency perturbations are imposed.
119

MESOPAUSE TEMPERATURE UNDER GLOBAL CLIMATE CHANGE FROMLONG-TERM OBSERVATIONS AND MODEL SIMULATIONS
Igor Mokhov1,2, Anatoliy Semenov1, Evgenii Volodin3, Maria Dembitskaya1
1

Obukhov Institute of Atmospheric Physics RAS, Moscow, Russia
Lomonosov Moscow State University, Moscow, Russia
3
Institute of Numerical Mathematics RAS, Moscow, Russia
2

mokhov@ifaran.ru

Coherences of temperature variations near mesopause from long-term measurements at theZvenigorod Scientific Station of the Obukhov Institute of Atmospheric Physics RAS in 1960–
2015 with solar variability and with variations of surface air temperature are analyzed. Together
with variations of temperature at the mesopause Tms from measurements of the hydroxyl
emissions we analyzed the temperature variations near mesopause Tm reduced to the same levelof solar activity. The observed strong decrease in temperature near mesopause during last
decades, particularly in winter, with its tendency to slow down since the 1980 s was detectedagainst the background of general increase in the surface air temperature of the Northern
Hemisphere TNHs and the Earth as a whole. It was revealed a sharp drop in winter temperaturenear mesopause in 1970 s and its synchronicity with the shift in climatic conditions at the surface
associated with changes in formation of El-Niño events and their impact on the global climate.
This temperature shift is more clearly manifested for Tm than for Tms. The general significant
negative correlation of temperature variations near mesopause and surface air temperature for the
Northern Hemisphere detected from 56-year observational data was not accompanied by any
significant coherence between the most long-period temperature variations from the crosswavelet analysis. To assess the possible manifestation of this coherence the results of numericalsimulations with a global climate model were used. According to model simulations for the
20–21 centuries taking into account anthropogenic forcings for significant coherence between
long-term variations Tm and TNHs the prolonged observations are required for temperature nearmesopause — about a century or more.
EXCITED COMPONENTS OF THE ATMOSPHERE AS THE POSSIBLE CAUSE
OF LIDAR BACKSCATTERING IN THE MESOSPHERE AND UPPER ATMOSPHERE
Vasily Bychkov, Andrey Perezhogin, Ilya Seredkin, Boris Shevtsov
Institute of Cosmophysical Research and Radio Wave Propagation FEB RAS, Paratunka, Russia
vasily.v.bychkov@gmail.com

The results of two-frequency lidar sounding of the atmosphere from the altitudes of 25–
400 km are presented. The data were obtained in 2008–2016 at a lidar site located in Kamchatka.
One lidar channel is applied to investigate the aerosol formations in the middle atmosphere andto record the resonance scattering on excited ions of atomic nitrogen in the upper atmosphere.
Nd:YAG laser operating on the wavelength of 532 nm is used in this channel. A dye laser withtunable frequency is applied in the second channel. The wavelength corresponds to the chosen
dipole transition between the excited states of atomic oxygen. The possibility of reconstruction of
excited atomic oxygen Nh-profile is shown. It may give information on precipitated electron spectra.
The methods for the measurement of background signals and for consideration of photomultiplierpulse effects useful for the lidar investigation of the upper atmosphere are described. Possible
manifestations of the resonance scattering in the region of the mesosphere are discussed.
120

THE SOLAR UV OBSERVATIONS IN ANTARCTICA(NOVOLAZAREVSKAYA STATION)
IN THE GROWTH PHASE OF THE 24TH SOLAR ACTIVITY CYCLE
Serge Shapovalov, Oleg Troshichev
Arctic and Antarctic Research Institute, St. Petersburg, Russia
olegtro@aari.ru

Spectral measurements of the UV irradiation were carried out in zenith of free atmosphere at
the station Novolazarevskaya (Antarctica) with spectrometer AvaSpec-2048 (www.avantes.com)
in 2008–2015. The results of spectral measurements revealed the strong UV fluctuations in rangeof 297–330 nm, which are related to solar cosmic rays and solar radio-emission making strong
impact on the upper mesosphere parameters, such as altitude and magnitude of mesopause, theice water content, the ozone content, and other mesopause constituents (AIM,[http://aim.hamptonu.edu]). Time series analysis of the daily mean standard deviation (SD) for
the UV fluctuation intensity in the summer local season demonstrates that the UV fluctuations
are linearly connected with radio-emission over the range 245–8800 МГц[http://www.sws.bom.gov.au]. The maximal correlation (R~0.9) takes place for the lowfrequency (245 MHz) radio-emission from solar corona, which intensity does not demonstrateobvious dependence on the solar activity cycle, in contrast to the high-frequency (>2800 МHz)
radio-emission from solar chromosphere. These results strongly suggest that state of the upper
mesosphere can be related to other factors than the solar activity variations.
GEOMAGNETIC ACTIVITY SIGNATURE
IN MESOPAUSE TEMPERATURE OVER YAKUTIA
Galina Gavrilyeva, Peter Ammosov, Anastasiya Ammosova, Igor Koltovskoi, Vera Sivtseva
Institute of Cosmophysical Research and Aeronomy SB RAS, Yakusk, Russia
gagavrilyeva@ikfia.ysn.ru

OH excitation (87 km) and its connection with geomagnetic activity was studied. The
measurements were performed by an infrared spectrograph at the Maimaga station (63° N,
129.5° E). The nightly averaged rotational temperatures of OH(6-2) obtained from 1999 to 2015
were considered. As a proxy of geomagnetic activity, the index Ap was taken. The maximum of
the solar activity was about two years ahead of the maximum temperature of the mesopause. The
fluctuation of the seasonally averaged temperatures (from August to May) correlated with theinter-annual change in geomagnetic activity. The correlation coefficient was R=0.51–0.1(p<0.05). The temperature data was divided into high geomagnetic activity (Ap>8) and low
geomagnetic activity (Ap<=8) years. Then the time series of each group was superposed by dayof year, and daily averages for the same day of year were calculated. We found hat in the years
with high activity the temperature of winter mesopause is about 10 K higher than in years withlow activity. In autumn and spring, there is no dependence of temperature on the level ofgeomagnetic activity. Work was funded by the grant No. 17-05-00855 of the Russian Foundationfor Basic Research.

121

THE PERFORMANCE OF THE TEC INPUT OPTION OF THE IRI-PLAS MODEL
AT TWO EQUATORIAL STATIONS
Shola John Adebiyi, Babatunde Olufemi Adebesin, Stephen Oluwole Ikubanni,
Benjamin Wisdom Joshua
Landmark University, Omu-Aran, Kwara State, Nigeria
johndat2003@gmail.com

One major application of ionospheric models such as the International Reference
Ionosphere (IRI) model is to evaluate the environmental effects on spaced-based
communications and navigation systems. In the IRI extended to the plasmasphere (IRI-Plas)model, the height limitation of the IRI model is overcome and also the modeling framework is
capable of assimilating measured value of some ionospheric observables into it, thus capturing
the dynamics of the ionosphere. In this paper, the results of the investigation of the performanceof total electron content (TEC) assimilative option of the IRI-Plas model over the “no input
option” at two equatorial stations during quiet and disturbed conditions was presented. The result
obtained showed that TEC predicted by the adaptation technique produced smaller error at theequatorial trough than near the crest for both quiet and disturbed periods. Also, there issubstantial improvement in storm-time predicted TEC. The prediction is however independent
on the storm’s severity. With TEC assimilation, the foF2 estimation error is generally
higher/smaller at the trough/crest for both quiet and disturbed conditions. IRI-Plas-hmF2
predicted with TEC adaptation option is poor at both locations during both quiet and disturbed
conditions. Consequently, in other to obtain a more realistic F2 layer peak parameters from the
IRI-Plas model, adapting the model alone to the TEC value may not be sufficient.
MITIGATION OF CHALLENGE OF RECALIBRATION OF SUNSPOT NUMBERS
USING PROXIES OF SOLAR ACTIVITY FOR THE IONOSPHERIC MODELS
Tamara Gulyaeva1, Feza Arikan2, Dieter Bilitza3
1

Pushkov Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation RAS,
Moscow
2
Department of EEE, Hacettepe University, Beytepe, Ankara 06800; Turkey
3
George Mason University, Fairfax, Virginia and NASA, GSFC, Greenbelt, Maryland, United States
gulyaeva@izmiran.ru

The International Reference Ionosphere (IRI) and its extension into the Plasmasphere (IRIPlas) are facing a challenge of misleading effects if used with the newly revised sunspot number,
SSN2, due to the fact that these models are developed using the predecessor SSN1 index. In thepresent study different solar activity proxy indices, such as F10.7 solar radio flux, EUV fluxes(26–34 nm, 0.1–50 nm), Lyman_a (121.6 nm) and MgII-core-to-wing-flux-ratio (280 nm) areconsidered as candidates for the model driving indices. The ionosonde-based IG-index is alreadyincorporated into IRI and the Global Electron Content (GEC) index is included by IRI-Plas assolar proxies for the F2 peak predictions. As a new option the Ionospheric Total ElectronContent (IT) index scaled to the pre-defined SSN1 time series is proposed based on GPS-derived
TEC-noon measurements at 288 IGS stations listed at http://www.izmiran.ru/ionosphere/
weather/tec/indexcur.html during the 23–24 solar cycles. This study is partly supported by
TUBITAK EEEAG 115E915.

122

FUSION OF IONOSONDE MEASUREMENTS AND TEC ESTIMATIONSUSING STATISTICAL TECHNIQUES
Ozan Koroglu1, Feza Arikan2, Cenk Toker2, Harun Artuner2, Zbysek Mosna3
1

Hacettepe University and ROKETSAN, Turkey
Hacettepe University, Turkey
3
Instituite of Atmospheric Physics, Academy of Sciences of the Czech Republic, Czech Republic2

arikan@hacettepe.edu.tr

Ionosphere is a plasma layer which extends between 60 and 1000 km in altitude. This
plasma structure has very complex characteristics depending on several effects such as solar andgeomagnetic activity. Satellite and HF communications directly affected from this structure. The
determination of statistical properties of ionosphere is very important for estimating the overallbehavior. One of the most important parameters for understanding ionosphere is Total ElectronContent (TEC) which is obtained from GPS measurements. Another way to measure ionosphericparameters is ionosonde measurements. Ionosondes are specialized sounding radars which‘measure’ the ionospheric parameters. Ionosonde stations are sparser than GNSS stations.
Therefore, the ionosonde measurements are less dense compared to TEC measurements fromGPS stations. The variability of the ionosphere can be identified using Probability Density
Functions (PDF). In this study, within-the-hour spatio-temporal characteristics of GPS-TEC, thecritical frequency of F2 layer, foF2, and maximum ionization height, hmF2, obtained fromionosonde measurements are described as a jointly parametric probability density function (PDF).
Due to the physical dependency of all parameters, the joint PDF can provide a description of thejoint relation between ionosonde measurements and TEC estimates that can result in a unified
structural representation of ionosphere at F2 layer. Statistical observations on joint PDF estimatesof TEC and foF2, hmF2 measurements of the ionosphere will contribute to developing virtual
ionosonde network model, which can further be used to derive virtual foF2 and hmF2 values.
SUITS/SWUSV: A SMALL-SIZE MISSION TO ADDRESS SOLAR SPECTRALVARIABILITY, SPACE WEATHER, EXTREME EVENTS AND SOLAR-CLIMATERELATIONSLuc Damé1, Alain Hauchecorne1, Slimane Bekki1, Mustapha Meftah1, Abdenour Irbah1,
Philippe Keckhut1, Eric Quémerais1, Alain Sarkissian1, Marion Marchand1,
Rémi Thiéblemont1, David Bolsée2, Nuno Pereira2, Gaël Cessateur2, Werner Schmutz3,
Margit Haberreiter3, Julian Gröbner3, Robert Wimmer-Schweingruber4, Steven Dewitte5,
André Chevalier5, Kanaris Tsinganos6
1

LATMOS/IPSL/CNRS/UVSQ, Guyancourt; France
BIRA-IASB, Brussels, Belgium
3
PMOD/WRC, Davos, Switzerland
4
CAU, University of Kiel, Germany
5
Royal Meteorological Institute of Belgium, Brussels, Belgium
6
University of Athens, Greece2

luc.dame@latmos.ipsl.fr

We present the SUITS/SWUSV microsatellite mission investigation: Solar Ultraviolet
Influence on Troposphere/Stratosphere, a Space Weather & Ultraviolet Solar Variability mission.
SUITS/SWUSV was developed to determine the origins of the Sun’s activity, understand the123flaring process (high energy flare characterization) and onset (forecast) of coronal mass ejections(CMEs). Another major objective is to determine the dynamics and coupling of Earth’s
atmosphere and its response to solar variability (in particular in the ultraviolet) and terrestrial
inputs. It therefore includes the prediction and detection of major eruptions and CMEs (LymanAlpha and Herzberg continuum imaging), and the solar forcing on the climate through radiations
and their interactions with the local stratosphere (ultraviolet spectral irradiance measurements from170 to 400 nm). The mission is proposed on a sun-synchronous polar orbit 18h–6h at 700–750 km(for almost constant observing) with a 7 instruments model payload of some 80 kg / 80 W:
SUAVE (Solar Ultraviolet Advanced Variability Experiment), an optimized telescope for FUV(Lyman-Alpha) and MUV (200–220 nm Herzberg continuum) imaging (sources of variability);
SOLSIM (SOLar Spectral Irradiance Monitor), a spectrometer with 0.5 nm spectral resolution
from 170 to 340 nm; SUPR (Solar Ultraviolet Passband Radiometers), with UV filter
radiometers at Lyman-Alpha, Herzberg, MgII index, CN bandhead and UV bands coverage up to
400 nm; HEBS (High Energy Burst Spectrometers), a large energy coverage (a few tens of keV
to a few hundreds of MeV) instrument to characterize large flares; EPT-HET (Electron-Proton
Telescope — High Energy Telescope), measuring electrons, protons, and heavy ions over a large
energy range; ERBO (Earth Radiative Budget and Ozone) NADIR oriented; and a vector
magnetometer. Complete accommodation of the payload has been performed on a small platformof PROBA type very nicely but could fit several others. Alternately or in complement, a small
coronagraph is also envisaged. Heritage is important both for instruments (SODISM and
PREMOS on PICARD, LYRA on PROBA-2, SOLSPEC on ISS,…) and platform (PROBA-2,
PROBA-V,...), leading to high technology readiness levels (>7). SUITS/SWUSV was initiallydesigned in view of the 2015 ESA/CAS (Chinese Academy of Sciences) Call for a Small
Mission; it is now envisaged for joint CNES/NASA opportunities or future European Calls for a
possible flight in 2022.
OBSERVATIONS OF DYNAMICS IN THE HIGH ARCTIC MESOPAUSE REGION
AND THERMOSPHERE
William Ward1, Marianna Shepherd2, Qian Wu3, Wayne Hocking4, Alan Manson5,
Chris Meek5, Sam Kristoffersen6, Chris Vail6
1

Department of Physics, University of New Brunswick, Canada
CRESS, York University, Toronto, Canada;
3
NCAR, Boulder, CO, United States
4
Western University, London, Ontario, Canada
5
University of Saskatchewan, Saskatoon, Canada
6
University of New Brunswick, Fredericton, Canada
2

wward@unb.ca

The Dynamics of the Neutral Thermosphere project is a multiple site, multiple instrument
observatory. The instruments are located in the Canadian Arctic at Yellowknife, Resolute Bay(75° N, 95° W) and Eureka (80° N, 85° W) and include meteor radars, high resolution
interferometers, and all sky imagers. Measurements include wind, temperature and airglow
irradiance at the latter two sites and a meteor radar at the former site. Inter-instrument and intersite comparisons of time series are being undertaken and provide insights into the dynamical
processes in the high Arctic mesopause region and thermosphere, and information on the various
observing techniques. Studies are under way, to determine whether common tidal and gravity
wave signatures can be observed at both sites and in the mesopause region and thermosphere.
Airglow irradiance, winds and temperatures are observed with several different instruments andcomparisons between the associated time series are revealing the consequences of the different
124observing processes. For example, Doppler shift wind measurements in airglow using
interferometers are irradiance weighted averages of the wind in each airglow layer whereas themeteor radar provides wind profiles. During the 8 years that the instruments have been taking
observations, several sudden stratospheric warmings have occurred. Similarities and differencesin wind, airglow and temperature time series between the different warmings will be summarized.

125

Session 7: DATA ARCHIVING AND ANALYSIS TOOLS_____________________________________________________________NCEI SUN TO EARTH: SPACE ENVIRONMENT ARCHIVE, TECHNIQUES,TOOLS AND RESULTS
Robert Redmon, William Denig, Arnaud Chulliat, Margaret Tilton,
William Rowland, Athanasios Boudouridis, Stefan Codrescu
NOAA/NCEI, United Statesrob.redmon@noaa.gov

The NOAA Solar Terrestrial Physics Program within the US National Centers forEnvironmental Information (NCEI) is dedicated to the observation and characterization of thenatural environment from Sun to Earth. NCEI’s environmental data sets from ground to orbital
platforms are vast in both space and time, with worldwide contributions of solar imagery,geomagnetic and ionospheric measurements and interpretations dating long before the1957/1958 International Geophysical Year (IGY). With technological advancements, continuous
operational measurements of the near-Earth space environment have trended towards the use of
fully instrumented space-based assets. Space platform measurements in NOAA’s current archive
provide (non-inclusively) irradiance measurements of the solar disk and plasma and magnetic
properties of the equatorial radiation belt charged particle environment sensed by the
Geosynchronous Operational Environmental Satellites (GOES), similar plasma properties andupper atmosphere energy inputs sensed by the low earth Polar Orbiting Environmental Satellites(POES), the European Meteorological Operational (MetOp), and Defense Meteorological
Satellite Program (DMSP; multi-institution collaboration) satellites. NOAA’s strong
observational commitment continues with two flagship programs: the Deep Space Climate
Observatory (DSCOVR) which provides NOAA with a new operational solar wind monitoring
capability, and the new GOES-R program (GOES-16 launched November 2016) which will
advance our solar observations and GEO radiation environment monitoring. The aggregatedexpertise within NCEI provides a powerful resource supporting many key, internationallyvaluable activities. These include leadership roles in cal/val and product development for GOESR and Swarm, the development of the standard International Geomagnetic Reference Field(IGRF), the World Magnetic Model and its Extension (WMM and EMM), several ionospherefocused products (e.g. the Swarm-based Dedicated Ionospheric Field Inversion (DIFI) model,
and automatic scalings of real-time ionograms), satellite anomaly investigations, NOAA’s foray
into the Big Data arena, and numerous contributions to the operations and research communities.
We present on the best practices and lessons learned, our new DSCOVR data extraction andvisualization portal, GOES-R analysis tools, new products and plans for advanced discovery,
visualization and dissemination, our geomagnetic and electric field products and services, andkey scientific results realized using our comprehensive Sun to Earth archives(www.ngdc.noaa.gov/stp/).

126

METHODICAL AND SOFTWARE TOOLS FOR THE PROCESSING
OF THE RAW DATA OF THE MAGNETIC OBSERVATORIES
Sergey Khomutov1, Oksana Mandrikova1, Igor Solovev1,2,
Ekaterina Budilova (Zhizhikina)1,2, Kusumita Arora3, L. Manjula3,
Phani Chandrasekhar3
1

Institute of Cosmophysical Research and Radio Wave Propagation (IKIR FEB RAS), Paratunka,
Kamchatka, Russia
2and Kamchatka State Technical University, Petropavlovsk-Kamchatsky, Russia
3
CSIR-National Geophysical Research Institute, Hyderabad, India
Khomutov@ikir.ru

The raw magnetic data obtained by regular observations at magnetic observatories are thebasis for research in many fields of science. The reliability, regularity and efficiency of the data
ensure the quality and effectiveness of researches, including in the field of the space weather
forecasts. Hardware developers with technical and technological advances provide observatories
with the wide range of digital magnetometers, the modern information and communication
systems of the data storage and database formation provide the scientific community with accessto the results of the measurements. Processing of raw data on the primary analysis step has asignificant importance. The report shows that much of this work cannot be delegated to the outerdata centers, and must be carried out directly at the observatories. First of all, this is due to theneed to consider local environmental factors that affect the results of the measurements, as well
as monitor the state of the equipment and make timely operational decisions for possible faults,
failures, etc. In spite of the intensive development of information and communication systems
and technologies, there are substantial gaps in methodological (to a lesser extent) and software(largely) support of the magnetologist workplace, which are being addressed in this work. The
authors developed specialized software system, including all stages of the processing of themagnetic data, since their primary analysis to high-tech mathematical methods for the study ofprocesses in the magnetosphere-ionosphere system. Much attention is paid to the creation ofeffective, reliable and user-friendly software for magnetologist, including procedures on
identification and removal of noise, control the baseline values, filling gaps in the data, as well as
the preparation of the final data with the status of Adjusted, Quasi-definitive and Definitive,
required by the INTERMAGNET standards. A significant part of the programs implemented andeffectively used at Paratunka, Khabarovsk, Magadan and Cape Schmidt magnetic observatories
of IKIR FEB RAS (Russia), testing the individual modules is performed at Hyderabad andChoutuppal observatories of CSIR-NGRI (India). This work was supported by Indo-Russia
collaborative project of RFBR No 16-55-45007.
DATABASE OF COSMIC-RAY NEUTRON FLUXES HELD BY WDC
FOR COSMIC RAYS
Takashi Watanabe
ICSU WDS International Programme Office, Tokyo, Japan
takashi.watanabe@icsu-wds.org

The World Data center (WDC) for Cosmic Rays was established in 1957 in RIKEN,Tokyo, as a C2 center of the ICSU WDC. This data center has been moved to the present
Institute for Space-Earth Environment Research, Nagoya University, in 1991. The principal data127

held by the WDC are pressure-corrected and scale-adjusted one-hour counts of cosmic-ray
neutron data since 1953 which are provided by ground-based stations (about 50 at present)
distributed in a wide range of the geographic longitude and the latitude. Data are opened throughthe Web page given below after fundamental quality control. This database will be useful forstudies of variations of cosmic-lay flux with time scales ranging from hours to years(http://center.stelab.nagoya-u.ac.jp/WDCCR/).
WDS ASIA-OCEANIA CONFERENCE, 2017
Takashi Watanabe
ICSU WDS International Programme Office, Japan
takashi.watanabe@icsu-wds.org

The World Data System (WDS) of ICSU will promote the conference entitled WDS AsiaOceania Symposium, 2017 to be held in Kyoto, Japan, from 26 to 28 September 2017. The
associated workshop on data analysis of current solar-terrestrial events will be held also on 25
September 2017 through the collaboration with the VarSITI community of Japan. Details on theconference are posted at http://wdc2.kugi.kyoto-u.ac.jp/wds2017/. WDS is an interdisciplinary
body of the International Council of Science (ICSU) whose mission is to promote international
collaborations on long-term preservation and provision of quality-assessed research data and dataservices across a range of disciplines in the natural and social sciences. Among 90 members of
WDS at present, only 14 members have been enlisted from the Asia-Oceania area. Increase thenumber of WDS members in this area is one of the principal action items of WDS because thisarea is important in various research disciplines, including solar-terrestrial science. Although
WDS has been evolved from the World Data Center (WDC) system established in the IGY era, anumber of former WDC members, particularly in China and Japan, have faced to difficulty to bemembers of WDS due to various reasons, including the change of interest of hostingorganizations. Establishment of a system to assure long-term preservation and provision of theirdata holdings is urgent. In addition, infrastructures of data management in the Asia-Oceania region
are still in the stage of development, instead of importance of this region in the Future Earthprogram of ICSU. In this conference, we will discuss on future actions to enforce collaboration.
IUGONET TOOLS FOR SOLAR-TERRESTRIAL PHYSICS RESEARCH
Yoshimasa Tanaka1, Norio Umemura2, Shuji Abe3, Atsuki Shinbori4,
Satoru UeNo5, Masahito Nose6
1

National Institute of Polar Research, Tokyo, Japan
Institute for Space-Earth Environmental Research, Nagoya University, Aichi, Japan
3
International Center for Space Weather Science and Education, Kyushu University, Fukuoka,
2

Japan

4

Institute for Space-Earth Environmental Research, Nagoya University, Aichi, Japan
Kwasan & Hida Observatories, School of Science, Kyoto University, Kyoto, Japan
6
Data Analysis Center for Geomagnetism and Space Magnetism, Graduate School of Science,
Kyoto University, Kyoto, Japan5ytanaka@nipr.ac.jp

We present useful tools for solar-terrestrial physics (STP) research, developed by Interuniversity Upper atmosphere Global Observation NETwork (IUGONET) project. IUGONET is aJapanese inter-university project that aims at developing infrastructure to share upper128

atmospheric data, including solar and planetary data, which have been separately archived by
Japanese universities and institutes, and to promote interdisciplinary studies on STP. We havedeveloped two tools, i.e., a metadata database and an analysis software for the upper atmosphericdata. Our metadata database, called IUGONET Type-A, allows users to cross-search various
kinds of the upper atmosphere data distributed across the IUGONET members. It provides a onestop web service to search data, show metadata and quick-look (QL) plot of the data, findinteresting STP events, interactively examine the data, and lead users to more detailed data
analysis by using our analysis software. Our analysis software is based on Space Physics
Environment Data Analysis Software (SPEDAS) that is a grass-roots software written byInteractive Data Language (IDL) and is capable of dealing with data from multiple missions. We
have provided a plug-in tool for SPEDAS, which enables analysis of data from the ground-based
observations by solar telescope, ionospheric and atmospheric radars, imagers, riometers,
magnetometers, etc. with SPEDAS. Since we are collaborating or are planning to collaborate
with several science projects such as ERG, PWING, Pulsating Aurora Project, EISCAT_3D,
Equatorial MU radar, and so on, the data from these projects will be further available in our tools.
In addition, we hold tutorial seminars to explain how to use these IUGONET data and tools inJapan and sometimes foreign countries several times a year. We believe that these tools areuseful for the Variability of the Sun and Its Terrestrial Impact (VarSITI) program, in particular,
Specification and Prediction of the Coupled Inner-Magnetospheric Environments (SPeCIMEN)
and Role Of the Sun and Middle atmosphere thermosphere/ionosphere in Climate (ROSMIC).

IRNSS/GPS DATA ANALYSIS FOR IONOSPHERIC STUDIES AT SANGLI(LATITUDE: 16º51’ N, LONGITUDE: 74º34’ E)
Dadaso Jaypal Shetti1, Trushali Suresh Vasagade2, Manali Sagar Manjarekar112Smt. Kasturbai Walchand College, Sangli, India
Annasaheb Dange Collegeof Engineering and Technology, Ashta, India

shettidj2002@yahoo.co.in

Data archiving plays significant role in the field of space communication, space weather
studies etc., as this archived data is an only source to gather desired information as per the predefined
objectives of respective system. Dedicatedly designed receivers for particular satellite system will
receive the signal from satellites. IRNSS data lot of seven days from extracted files can be selected
and proceed further with IRDAS software which will generates plot of each satellite existing insystem in various manners and for different parameters. IRDAS initially deals with the reference
position of receiving station so as to generate an output. Hence, real time data logging and its weekly
record maintaining will be achieved by these sophisticated software’s The proposed project
objectives demand to have some more and different parameter to archive and proceed than IRDAS
tool. Hence, paper presents estimation and its preliminary results of comparative analysis of
ionosperic delay and TEC from IRNSS/GPS/SBAS data using different softwares.

129

CURRENT STATUS OF CATALOG OF LARGE-SCALE SOLAR WIND PHENOMENA
Irina Lodkina, Yuri Yermolaev, Nadezhda Nikolaeva, Michael Yermolaev
Space Research RAS, Moscow, Russia
irina-priem@mail.ru

During 2002–2007 we prepared a method of identification of large-scale solar windstructure on the basis of OMNI database of 1-h solar wind (SW) plasma and IMF parameters andwe have made the “Catalog of large-scale solar wind phenomena for period 1976–2000” (seewebsite ftp://ftp.iki.rssi.ru/pub/omni/ and paper [Yermolaev et al., 2009]). Our catalog identifies
reliably 3 types of quasi-stationary streams of the solar wind (heliospheric current sheet (HCS),
high speed streams from the coronal holes (HSS), and slow streams from the coronal streamers),
and 5 disturbed types (compression regions before fast streams HSS (CIR), and interplanetary
manifestations of coronal mass ejections (ICME) that can include magnetic clouds (MC) andEjecta with the compression region Sheath (SHEMC and SHEEj) preceding them) as well as theinterplanetary shock (IS). In the report we will described the procedures of SW typeidentification, data processing and visualization, and web site using. Current status (27 February,
2017: Calculation of parameters 1976–2015, Visualization of parameters 1976–2015,
Identification of SW types 1976–2005, 2011–2015, Visualization of SW identification 1976–
2005, 2011–2015. The work is supported by the VarSITI grant.

PROGRESS IN HANDLING AND ANALYSIS OF GROUND-BASED GEOMAGNETICDATA STREAMS FOR ADVANCED MONITORING OF THE EARTH’S MAGNETIC
ENVIRONMENT
Anatoly Soloviev
Geophysical Center RAS, Moscow, Russia
a.soloviev@gcras.ru

The continuous growth of geophysical observations requires adequate methods for theirprocessing and analysis. On the other hand, geomagnetic studies require accurate and reliablemeasurements of the Earth’s magnetic field (EMF) carried out from ground and space. The
system analysis methods and data mining techniques are able to sustain the solution of these
problems. This paper presents an innovative holistic hardware/software system developed for
efficient management and intellectual analysis of geomagnetic data, registered by Russian
geomagnetic observatories. The designed system provides sophisticated automatic detection andmulti-criteria classification of extreme geomagnetic conditions, which may be hazardous fortechnological infrastructure and economic activity in Russia. The geomagnetic activity indicators
include measure of anomalousness (MA), rate of change and amplitude of the geomagnetic fieldand near real-time K index. An essential feature of the developed system is its ability to deal
continuously with real time data streams. It enables the online access to digital geomagnetic dataand its processing results along with its visualization on conventional and spherical screens. In
addition to recognition of increased magnetic activity, the fuzzy-logic based MA indicator isdually used for defining magnetically quiet periods. This feature makes the MA applicable forselecting quiet days and consequently more precise and timely determination of Sq variations at
specified observatories, as compared to classical IAGA approach. This method also plays
130

important role in selection of observatory data for constructing proper geomagnetic field models
of internal origin. With this respect, we give a description of the principally new approach to
calculating magnetometer calibration values (baseline estimations), which is a crucial operationin producing continuous high quality measurements of the complete field vector at geomagnetic
observatories. As opposed to the baseline estimation method, traditionally accepted in
INTERMAGNET, this approach involves all information on the geomagnetic field variations(both, vector and scalar), available in between infrequent absolute measurements taken byobservatory operators. As a result, it provides information on the observatory data errors, whichis especially important in robust modeling of rapid core magnetic field variations. Secularvariations (SV) of the EMF on short time intervals are detected by calculating the second time
derivative (secular acceleration, SA) of the field. However, charting the SV and SA at the coremantle boundary that might reveal sudden changes of SA polarity happening within a year or sois only possible for models derived from recent, high accuracy satellite observations. We propose
a new way to SV modelling and detection of SA pulses that are direct manifestation of the
dynamic processes in the liquid core, using observatory data solely. It enables retrospective
historical data processing for recognition of SA pulses and geomagnetic jerks before 2000, whenfull-scale geomagnetic satellite observations started.

RESULTS FROM FY-3 SOLAR IRRADIANCE MONITOR OBSERVATION,
A NEW TSI DATA RECORD
Jin QiNational Satellite Meteorological Center, China meteorological Administration, Beijing, China
qijin@cma.gov.cn

FengYun (FY)-3 satellites are the second generation of Chinese polar-orbiting
meteorological satellites. The main goal of FY-3 is the measurement of three-dimensional,
multi-spectrum and global remote sensing under all weather conditions. It could provide theapplication on weather monitoring and forecasting, earth radiation budget and climate change
et.al.The Solar Irradiance Monitor (SIM) is aim to capture variation of solar energy at the whole
waveband from the top of atmosphere with Total Solar Irradiance (TSI).It is designed for climate
research coupled with Earth Radiation Measurement together as an instrument group and began
to work from June, 2008.. With the experiences from the first two satellites, the SIM on FY3C
has two significant improvements by adding sun tracing system and temperature control system,
which is named after SIM-II.TSI from FY3C/SIM-II has been evaluated by comparing with
SORCE/TIM and RMIB composite data. The result shows a good consistency. Monitoring ofstrong solar activity during Oct. 2014, FY3C/SIM-II and SORCE/TIM showed the same level
about solar energy change. This work shows the new results from recalibrated SIM TSI data
record after improvement on background and aging correction and its capability on monitoring
solar activities.

131THE TECHNIQUE FOR ESTIMATION OF ABSOLUTETOTAL ELECTRON CONTENT USING DUAL-FREQUENCYAND SINGLE-FREQUENCY GPS/GLONASS DATA
Anna Mylnikova1, Yury Yasyukevich1,2, Vsevolod Ivanov2
12Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
Irkutsk State University, Irkutsk, Russia

manna@iszf.irk.ru

We have developed a technique for total electron content (TEC) estimation from the dualfrequency and single-frequency data of an individual GPS/GLONASS station. Estimating isbased on dual-frequency data of phase measurements and single-frequency GPS/GLONASS dataof joint phase and group pseudorange measurements. The algorithm is based on TEC Taylor
series expansion in space and time (TayAbsTEC). The validation was performed based on datafrom Global Ionospheric Maps (GIM) by CODE and JPL. We compared differences between
absolute vertical TEC (VTEC) from GIM and VTEC evaluated by TayAbsTEC based on dualfrequency data. for solar minimum(full 2009), and for solar maximum (full 2014). It was foundthat the difference between JPL VTEC and VTEC by TayAbsTEC higher than the difference
between CODE VTEC and VTEC by TayAbsTEC. The difference is higher for solar maximum(2014) as compared with solar minimum for both CODE and JPL. Also we compared singlefrequency technique result with dual-frequency those. Estimated single-frequency vertical TEC
agrees qualitatively and quantitatively with the dual-frequency vertical TEC. A typical value ofthe difference between the single-frequency vertical TEC and the dual-frequency one for the
analyzed stations generally does not exceed ~1.5 TECU with RMS up to ~3 TECU. The
distribution of VTEC differences has the form of a Gaussian distribution. Results of TayAbsTEC
are in the agreement with GIM VTEC. The developed technique can be used for VTEC calculation
based on dual-frequency or single-frequency GPS/GLONASS data from local stations.
THE IONOSPHERIC DYNAMICS AS MEASURED BY THE DOPPLER SOUNDING
AND BY THE DIGISONDE TECHNIQUE
Daniel Kouba, Jaroslav Chum
Institute of Atmospheric Physics CAS, Czech Republickouba@ufa.cas.cz

Vertical ionospheric sounding produces ionograms and subsequently electron density
profiles. Modern ionosondes arealso able to monitor dynamics of ionospheric layers by drift
measurements. The drift measurements have been performed at ionospheric observatory of
Pruhonice for the last 10 years with 15 min cadence. Since 2007, Continuous Doppler Sounding
have also been carried out to monitor wave activity on short timescales, up to ~10 s. Both
Digisonde and Continuous Doppler Sounder measure about the same volume in the ionosphere.
Our contribution compares the potential of both measurements to investigate dynamics of theionosphere. Several case studies are presented. Monitoring of the dynamics of the ionosphere has
great potential for the prediction of ionospheric conditions.

132

KONUS-WIND HARD X-RAY AND SOFT GAMMA-RAY SOLAR FLARE DATABASE
Alexandra Lysenko1, Rafail Aptekar1, Gregory Fleishman2, Dmitry Frederiks1,
Larisa Kashapova3, Alexey Kuznetsov3, Anastasia Tsvetkova1, Mikhail Ulanov1,
Zinaida Sokolova1, Dmitry Svinkin1, Philipp Oleynik1, Alexey Kokomov1
1

Ioffe Physico-Technical Institute RAS, St. Petersburg, Russia
New Jersey Institute of Technology, Newark, United States
3
Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
2

alexandra.lysenko@mail.ioffe.ru

Konus-Wind is a joint US-Russian experiment for gamma-ray burst and solar flare studies.
The experiment started on November 1, 1994. Being located in the interplanetary space (since
July of 2004 — near Lagrange point L1) Konus-Wind doesnt suffer from “nights”. During its
more than 22 year-long history Konus-Wind has accumulated a unique volume of solar flareobservations in hard X-ray and soft gamma-ray range. Data registered by Konus-Wind in thetriggered mode constitute the presented database, named KW-Sun. The data can be accessed via
http://www.ioffe.ru/LEA/kwsun/ (at the time of writing the data for years 2005-2017 areavailable, the remaining data will be added soon). New solar observations will be added to the
database as soon as they arrive. KW-Sun provides light curves with high temporal resolution(down to 16 ms) and energy spectra in wide energy range (now ~20 keV – 15 MeV) which
covers the region of non-thermal emission from electrons and ions accelerated in solar flares. We
present some statistics describing solar flares observed by Konus-Wind and compare flare
properties between solar cycles 23 and 24.

INTERFERENCES ON THE CORRELATION DATA OF THE SIBERIAN
RADIOHELIOGRAPH
Veronika Kobets
Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
Veronikakobets@yandex.ru

The first phase of the Siberian Radioheliograph (SRH) is a 48-antenna array. One type ofradioheliograph data represents correlation plots. In evaluating the covariation of two-levelsignals, these plots are sums of complex correlations, obtained for different antenna pairs.
Bearing in mind that correlation of signals from an antenna pair is related to a spatial frequency,
we can say that each value of the plot is an integral over a spatial spectrum. Limits of theintegration are defined by a task. Only high spatial frequencies are integrated to obtain dynamics
of compact sources while the whole spectrum is integrated to reach maximum sensitivity. These
data are affected by the some interference: the radio emission of the geostationary satellites forthe about 0 declination, the forest emission especially for negative declinations. In this work weshow how to mitigate the influence of these interferences on the correlation plots of the SRH.

133

MODELING INTERFEROGRAM IMAGES FOR THE OUTPUT DATA SIMULATIONOF FABRY–PEROT INTERFEROMETER
Maksim Artamonov, Roman Vasilyev
Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
artamonov.maksim@iszf.irk.ru

The determination of winds and temperatures in thermosphere is quite important for global
atmospheric model developments. One of the instrument used for solving such a task is an
imaging Fabry–Perot Interferometer (FPI). This study is devoted to the simulation of 2D images
for Keo Scientific Arinae FPI equipped with CCD sensor. The numerical process was based on
calculating an integral sum of Airy function as an apparatus function of FPI with the weights
defined as Gauss distribution function of a source spectrum. To approach the reality, scattering,
vignetting and other deviations from the ideal apparatus function were taken into account. Twotypes of images were made during the simulation: “He-Ne laser” calibrating interferograms at
the wavelength λ=632.8 nm and “sky” interferograms for observing the emission caused by the
dissociative recombination of O_2^+ with the wavelength λ=630 nm. The latter images had a
Doppler shift and broadening of spectrum connected with the emulated wind and temperature
respectively. The simulated pictures were processed by FPI handling software (FPIHS). The
values of wind, temperature, intensity and background restored with this software were found to
be in good correlation with the parameters used in simulating. Also, the experiments withincreasing noise were carried out for the signal noise ratio (SNR) resolution limit determinationof FPIHS. In addition, the images for a composite spectrum with varied intensities of input
emission containing contamination of O+ and OH lines were simulated and processed by FPIHS.
This resulted in decreasing temperature measured when the OH line was stronger but its local
increasing when the intensities were equal. All the aforementioned were done assuming thehomogeneous distribution of winds and temperatures in the observation field. Moreover,studying the heterogeneous distribution of winds and temperatures for further research was
begun. This includes the simulation of small regions with particular wind and temperature in thefield of observation with different wind and temperature values.The data used in this work wereobtained from FPI included in CCU “Angara”.This research was carried out with the support offinancial funds of “Studying dynamic processes in neutral atmosphere—ionosphere—
magnetosphere of the Earth”, project UN 0344-2014-0006. RN CITIS – 01201281656.
A STUDY OF POSSIBILITIES OF “GNU RADIO COMPANION”
FOR CHIRP SIGNAL PROCESSING
Andrew Naumenko, Anton Kim, Vladimir KurkinInstitute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
naym@iszf.irk.ru

This paper shows the possibilities of the GNU Radio Companion for signal processing.
The GNU Radio Companion is free software for working with various signals such as data from
SDR (Software Defined Radio) receivers or data from sound card. Using the digitized output
signal from the receiver (Icom IC-R75) ionograms were constructed. Methods for improving thequality of the received data using the built-in functions of GNU Radio are considered. At sametime, data from this receiver are obtained by standard, paid software. At the end, the obtained
data were compared. It was shown that the GNU Radio Companion software can be used forchirp signals processing, which are using to diagnostics of ionosphere.
134

METEOR TRAIL OBSERVATIONS AT EKB ISTP SB RAS RADAR.
Roman Fedorov, Oleg Berngardt
Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia
fedrr@iszf.irk.ru

This work is based on coherent decameter radar EKB ISTP SB RAS (8-20MHz) locatednear Ekaterinburg. EKB is over-the-horizon radar with 50 degrees field-of-view sliced into 16
beams, with 15–45 km spatial resolution and 1–2 min time resolution over field-of-view (of 4–8 sec
at single beam) in normal operating mode. In normal mode the radar transmit series of multipulse sequences (7–16 pulses in each sequence depending on sounding mode), then calculate an
autocorrelation function (ACF) of the received signal for every range gate and accumulates themover several (~40) sounding sequences. In this paper we use raw data — quadrature (IQ)
components of the received signal. Using this data becomes possible to study scattering frommeteor trails (burning heights ~ 80–100 km). Monitoring of meteor echos is a common operating
mode for the most part of SuperDARN radars, similar to EKB radar. The algorithms used in thismode are based on analysis of ACF, and time resolution is about 4-8 seconds. We implemented
an algorithm that searches for meteor echos in IQ components of scattered signal. This allows us
to reach time resolution up to 5 milliseconds. Algorithm is based on exhausting search of model
parameters: meteor trail life-time and Doppler drift to find a pair with least mean squaredeviation with experimental data. Optimal model parameters allows to calculate thecharacteristics of meteor trail: azimuth, distance, meteor lifetime and line-of-sight velocity. The
algorithm uses standard radar output files and can work in real time during radar operation.
Algorithm had been implemented on EKB radar since December 2016 and used as common
real-time radar data processing method. Also it can be used for retrospective data analysis. The
meteor trail characteristics obtained from the radar data can be used to study the neutral
atmosphere dynamic. In this paper we present the first statistical analysis of meteor trail
characteristics over EKB radar data since early 2016 until now. The diurnal and season variation
are also presented.
IRI-PLAS WITH TEC ASSIMILATION AS AN ONLINE SERVICE AT IONOLAB
Feza Arikan1, Tamara Gulyaeva2, Umut Sezen1
1Hacettepe University, Turkey
Pushkov Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation RAS,
Moscow, Russia
2arikan@hacettepe.edu.tr

International Reference Ionosphere (IRI) is a joint task group of COSPAR and URSI,
which is dedicated to provide a reliable and accurate climatic model for structural parameters of
ionosphere. IRI is an empirical and deterministic model that uses hourly monthly medians of F2
layer critical frequency, foF2. IRI is originally developed in FORTRAN language and currently,
it is available at http://irimodel.org/ with an online version. The IRI model can provide electron
density profile, layer parameters and ion and electron temperatures in the general range of 80 to
2,000 km. Users can specify the location, date, time and the height profile boundaries for a single
run. The outputs can be obtained in the text format or the profiles or distributions can be drawn
according to user specifications. IRI is accepted as the international standard model ofionosphere. IRI Extended to Plasmasphere (IRI-Plas) is a recently developed version of IRI
model by Dr. Tamara L. Gulyaeva of IRI task group. In IRI-Plas, the region of interest can
135include the plasmasphere up to the GPS satellite orbital height of 20,200 km. IRI-Plas provides
structural model of ionosphere up to plasmasphere in regions where ionosonde data are notavailable. IRI-Plas is available as a FORTRAN code at ftp://ftp.izmiran.rssi.ru/pub/izmiran/
SPIM/. IONOLAB Group has been using IRI-Plas as a basis of various research products
provided in www.ionolab.org as space weather services such as IRI-Plas-MAP, IRI-Plas-STEC,
and algorithm for computerized ionospheric tomography, namely, IONOLAB-CIT, and novel
electromagnetic wave propagation algorithm in ionosphere, IONOLAB-RAY. In order tofacilitate the usage of IRI-Plas for other possible users, IONOLAB group has implemented theonline version at www.ionolab.org. The input page and the output of the program are similar to
the internet access page of IRI-2016. The most important aspect of Online IRI-Plas is theautomatic assimilation of Global Ionospheric Map (GIM) Total Electron Content (TEC). The
user can also supply the TEC by typing in the value in the designated slot. Also, the user can run
the algorithm with various input sets in a batch which is an advantage to avoid multiple runs.
The user friendly online IRI-Plas algorithm allows for ionospheric modeling up to the height
20,200 km for any ionospheric state, date, time and location. This study is supported by grantfrom TUBITAK EEEAG 115E915 project.
APPLICATION OF A ROBUST CRITERION FOR FILTERING TIME SERIESOF IONOSPHERIC PARAMETERS
Inna Belashva, Vladimir Bochkarev
Kazan Federal University, Kazan, Russia
inkin91-91@mail.ru

Nowadays filtering is widely used as a method of data processing. Frequency filtering has
been studied quite well, and there are many algorithms and methods of such filtering (spectral
analysis). However, at the present time, filtering, based on statistical significance is becoming
popular, the simplest example of which is wavelet filtration, where the criterion of quality is theminimum root-mean-square error. Such a criterion gives excellent results for data whose
probability distribution is described by a Gaussian law. Unfortunately, for data with a different
distribution, this approach may not be correct. So, the development of a universal sustainable
criterion becomes an urgent problem. One of the most famous universal criterion is the
maximum likelihood method, which, however, requires knowledge of the type of distribution forrecording the quality criterion. Here there are two key difficulties: Distribution is not always
known;It is rather difficult to record the quality function for some types of distribution.Suchcomplexity can be circumvented, using as a criterion of quality a criterion that does not dependon the type of distribution. The series criterion is one of them - in this case the RamachandranRanganatan criterion was used, which is written as follows: The filtering in this case will bebased on the minimum amount of squared series length multiplied by the number of suchseries,assuming that random events do not organize long series, thereby allowing to separate
meaningful signals from random ones. To minimize the error, it is suggested to use genetic
algorithms — one of the stochastic optimization methods. To compare the filtration methods, theseries were modeled, with different distribution of the noise component. The results of filteringby different methods showed the advantage of the serial criterion over the criterion of theminimum mean square error. Also these algorithms were used for filtration of temporary ranks ofionospheric parameters, namely ranks of critical frequencies of a layer of F2 to searchquasiperiodic variations. Results of such researches also showed advantage of serial criteria.

136

CAPABILITIES OF MOBILE ROBOTS TO MAP ELECTROMAGNETIC RADIATION
OF LITHOSPHERIC ORIGIN
Vladimir Mochalov, Vladimir Uvarov
Institute of Cosmophysical Research and Radio Wave Propagation FEB RAS, Russia
sensorlife@mail.ru

The main aim of the work is the construction of a system for mapping of electromagnetic
radiation of lithospheric origin (ERLO) based on the application of a self-organizing wirelesssensor network (SWSN). When solving the problem, we assume that an object for ERLO
mapping is known, the number of measurement points is not exactly defined and deliberately
exceeds the number of network sensors. The problem is assumed to be solved by mobile robots(drone, ground, above- and under-water vehicles). Mobile robots are applied as intelligent agentsand form a distributed multi-agent system based on the SWSN. Some functions of mobile robots
are: construction of self-organizing structures of antenna distribution; formation of a selforganizing wireless sensor network including ground and mobile segments; geographicallydistributed acquisition of data from SWSN sites; organization of the interaction of a SWSN
mobile segment with a ground one; distributed registration of electromagnetic radiation in agiven area; accurate arrangement, distribution over a territory, movement, removal,
reprogramming, charging and replacement of power sources at SWSN sites; planning ofcooperative behavior of mobile robots in the process of solution of a SWSN functioning general
aim and reconstruction of SESN sites based on the aims and current measurements of the whole
SWSN. We can show the following stage process as one of possible examples of ERLO mapping.
At the first stage, the sensors measuring ERLO are arranged in priori or randomly chosen
positions (i.e. a SWSN ground segment is built) by mobile robots. During the following repeatedstages, ERLO preliminary distributions are estimated, ERLO distributions are mapped, ERLO
local maxima are determined, constant level lines and gradient lines of ERLO are drawn, thepositions appropriate for sensor location are calculated based on the obtained information,
SWSN sites are rearranged based on the aims and current measurements of the whole SWSN.
The process of data acquisition is stopped when the aim or a stop criterion is achieved. Possible
applications are monitoring of seismic activity, engineering facilities and exploration of minerals.

137

AUTHOR INDEXА
AbdelHady Ahmed Abdel
Abdullaev Alisher
Abdulrahim Rasheedat Bola
Abe Shuji
Adebesin Babatunde
OlufemiAdebiyi Shola John
Adeniyi Jacob Olusegun
Abunin Artem
Abunina Maria
Afanasyev Andrey
Afanasiev Nikolay
Akiyama SachikoAkchurin Adel
Aldás Franklin Bolívar
Alsatkin Sergey
Altyntsev Alexander
Ammosov Peter
Ammosova Anastasiya
Anfinogentov Sergey
Anil Kumar C.P.
Antokhin Pavel
Antokhina Olga
Aol Sharon
Aptekar RafailArikan Feza

34
109
71
128
122
122
71, 7599
99
24
68
10, 24, 104674562
19, 21, 25
121
121

Arora Kusumita
Artamonov Maksim
Artuner Harun

27
66
111
111
73
133
41, 54, 56, 122,
123, 135
79, 127
134
123

B
Babatunde Rabiu A.
Badeke Ronny
Baishev Dmitry
Bal Sourabh
Banerjee Dhruba
Bankov N.
Beddeley Lisa
Bekki Slimane
Belakhovsky VladimirBelashva Inna
Beletsky Alexander
Belov Anatoliy

84
79
77, 79, 86
108
3, 44
76
71
43, 47, 123
71, 80136
98
99

Benghin V.
Berngardt Oleg
Besliu-Ionescu Diana
Bessarab Fedor
Bezrukikh Vladilen

7668, 96, 135
1551
86, 87

Bhattacharyya Archana
Biktash Lilia
Bilitza Dieter

74
59, 114
122

Bochkarev Vladimir
Bolaji Olawale Segun
Bolsée David
Bondar Elena
Borchevkina Olga
Borodkova Natalya
Borries Claudia
Boudouridis Athanasios
Budilova (Zhizhikina)
Ekaterina
Buresova Dalia
Byalko Alexey
Bychkov Vasily

136
72, 8443, 47, 48, 123
89
51, 97
12
79
126
127

C
Cameron Robert Harold
Casti Marta
Cessateur GaëlChandra Ramesh
Chandrasekhar Phani
Chandrasekhar Phani
Chang Loren Cheewei
Chau Jorge
Chelpanov Andrei
Chelpanov Maksim
Chen Linjie
Chen Xingyao
Chen Zhijun
Cherepanova Lidiya
Chernigovskaya Marina
Chevalier André
Chi YutianChien Shih-Han
138

91
117
120

46
30
47, 123
6
79
127
52
112
14
14
28
29
28
58, 103, 113
60, 61123
652

Chirik Nikolay
Cho Young-Min
Chulliat Arnaud
Chum Jaroslav
Chupin Sergei
Cilliers Pierre
Cinar Ali
Clette Frédéric
Codrescu Mihail
Codrescu Stefan
Costa-Duarte Marcus
Criddle Neal56, 109
118
126
132
14
72
41, 56
39
118
126
17
59

D
Dadaso Jaypal Shetti
Dachev C.
Dalla Silvia
Damé Luc
Danov Dimitar
de Haro Barbas Blas
Deepak Kumar Sondhiya
Dembitskaya Maria
Demekhov Andrei
Dementeva Alla
Demetrescu Crisan
Denig William
Denisenko Valery
Deres Anastasiya
Despirak Irina
Devyatova Elena
Dewitte Steven
Dmitriev Alexei
Dumbrava Zinaida
D’Huys Elke
Dobrica Venera
Dumbović Mateja
Dzhalilov Namig Sardar

129
76, 123
25
43, 47, 48, 123
17, 11354, 55
5
120
83
113
41
126
53
23
16, 85111
123
55, 7691
16
41
102
20, 21

E
Edemskiy Ilya
Efendi Emre
Efishov Ivan
Egorov Yaroslav
Ejiri Mitsumu
Elango P.

64, 9141
97
8, 10, 1169
66

Elias Ana
Engebretson Mark
Entzian Günter
Eselevich Victor
Eselevich Maxim

38, 54, 55
80
112
12
12

F
Fainshtein Victor
Falayi E.
Fedorov Roman
Fedotova Anastasiia
Feynman Joan
Fleishman Gregory
Flores Ivaldi Gerardo
Frederiks Dmitry
Fritts David8, 9, 10, 11
84
135
25
35
133
38
133
59

G
Gaidash Sergei
Gatica-Acevedo Victor Jose
Gavrilov Nikolai
Gavrilyeva Galina
Gburek Szymon
Geng Lihong
Georgieva Katya
Cherepanova Lidiya
Ghodpage Rupesh
Gilbert Pierre
Gjerloev Jesper
Globa Mariia
Golikov Innokenty
Gololobov Artem
Golovko Aleksei
Golubeva Elena
Gonzalez-Esparza Juan
AmericoGopalswamy Nat
Goryaev Farid
Grach Veronika
Grechnev Victor
Grkovich Konstantin
Gröbner Julian
Gryciuk Magdalena
Gubin Alexey
Guineva Veneta
Gulyaeva Tamara
139

99
83
51, 107121
19, 31
28
17, 32, 42, 58
103
57
48
114
93
82
82
14
36
83
10, 24, 10415
83
18, 21, 25
96
123
19, 23, 31, 47
21
16, 85, 113
37, 122, 135

Gurram Padma
Gurubaran SubramanianGvozdarev Alexey

74
57
99

Č
Čalogović Jaša

102

H
Habarulema John Bosco
Haberreiter Margit
Hanslmeier Arnold
Hauchecorne Alain
Heber Bernd
Heredia Teresita
Hocking Wayne
Huang Jing
Hunt Linda Allen72, 91123
28
47, 123
102
38
124
29
112, 114

I
Ievenko Igor
Ikubanni Stephen Oluwole
Ilminskaya Alexandra
Inoue Satoshi
Irbah Abdanour
Ismayilli Rajab
Ivanov Eugene
Ivanov Vsevolod
Ivanova Vera77, 8612251
2243, 47, 48, 123
21
21
132
91

J
Joshua Benjamin Wisdom

75, 122

K
Kaifler Bernd
Kaka R.O.
Kakad Bharati
Kalegaev Vladimir
Kanekal Shrikanth
Karagodin Arseniy

59
84
74
105
105
117

Karatay Secil
Karlicky Marian
Karpachev Alexander
Karpov Ivan
Kashapova Larisa
Kassamba Abdel Aziz
Diaby
Katashevtseva Darya
Keckhut Philippe
Kelyuev Sumer
Kepa Anna
Keuer Dieter
Khabituev Denis
Khalipov Viktor
Khlystova Anna
Khomich Vladislav
Khomutov Sergey
Kilcik Ali
Kim Anton
Kirichenko Kiril
Kirillov Andrey
Kirov Boian
Kiselev Valentin
Kleimenova Natalya
Klibanova Yulia
Klimenko Vladimir
Klimenko MaximKnížová Petra Koucká
Kobanov Nikolai
Kobets Veronika
Kochanov Alexey
Kochugova Elena
Kogure Masaru
Kokomov Alexey
Koleva R.T.
Koltovskoi Igor
Kolmakov Alexandr
Koltunenko Luiza
Kondratev Andrey
Korenkova Nina
Koroglu Ozan
Kostarev Danila
Kotova Daria
Kotova Galina
Kouba Daniel
Kovadlo Pavel
Koval Andrei
Kovalenko Vladimir
Kovyazina Natalya
Kozelov Boris
140

41, 561956
51
21, 22, 133
53
64, 65
123
99
23
112
116
82, 8913
119
79, 127
42
134
40
113
42, 5818
16
65
55, 56, 109
55, 56, 87, 109
58, 6114
133
18, 21, 25
119
69
133
76
121
99
97
66
56, 109123
92
87
86, 87, 89
58, 61, 132
119
51, 10740
105
85, 101

Kozlovsky Alexander
Krastev K.
Kristoffersen Sam
Krivolutsky Alexei
Krupar Vratislav
Kruparova Oksana
Kryakunova Olga
Kshevetskii Sergei
Kucuk Furkan Ali
Kudryavtseva Anastasiia
Kurikalova Marina
Kurkin Vladimir
Kusano Kanya
Kuznetsov Alexey
Kuznetsova Tamara

L
Lakshmi Narayanan
Viswanathan
Lastovicka Jan
Lavygin Ivan
Lebedev Valentin
Ledentsov Leonid
Lefèvre Laure
Lemaire Joseph
Lemmerer Birgit
Lesovoi Sergey
Liley Ben
Lipko Iurii
Liu Fei
Liu Zhong
Lodkina Irina
Lubchich Andris
Lukin Vladimir
Lunyushkin Sergei
Lübken Franz-Josef
Lysenko Alexandra

M
Magdalenic Jasmina
Makela Pertti
Malchev S.
Maltseva Olga
Manali Sagar Manjarekar
Mandrikova Oksana
Manjula Lingala

61, 9276
124
58, 103, 113
16
16
99
51
75
17
66
68, 96, 13422
133110, 115

57

Manson Alan
Manuilova Rada
Marchand Marion
Markov Alexander
Marshall Thomas
Matsuda Takashi
Maurchev Eugeny
Medvedev Alexander
Medvedev Andrey
Medvedeva Irina
Meek Chris
Meftah Mustapha
Meshalkina Natalia
Meszarosova Hana
McKinnell Lee-Anne
McLaughlin Pattilyn
Mielich Jens
Mierla Marilena
Mikhalev Alexander
Mironova Irina

124
108
123
56, 109
112
69
57
69
62, 92, 94
63, 64, 98, 119
124
43, 47, 48, 123
4, 19
19
72
59
61
15
95, 9837, 11735, 91
96
96
7
39
86
28
19, 21, 25
59100, 102
28
3
130
16
119
66
45, 59133

Miroshnichenko Leonty
Mirtoshev Zavkiddin
Mishin Vilen
Mishin Vladimir
Miteva Rositsa
Mlynczak Martin
Mochalov Vladimir
Mokhov Igor
Molodykh Sergey
Monga Aabha
Mordvinov Alexander
Mordvinov Vladimir
Mosna Zbysek
Mrozek Tomasz
Muhamad Johan
Mulligan Tamitha
Muntean Georgeta Maris
Mylnikova Anna

39
33
66
65, 66
17
112, 114
137
120
40, 11527
36
111
58, 123
47
22
103
15
60, 61, 132

16
10, 24, 104
76
83
129
77, 79, 127
79, 127

N
Nakamura Takuji
Nakariakov Valery
Nagovitsyn Yuri
Naumenko Andrew
Nepolian Jeni Victor
Newell Patrick
Nikolaev Alexander69
26, 27
42
134
66
101
101

141

Nikolaeva Vera
Nikolaeva Nadezhda
Nikolayevskiy Nikolay
Nishiyama Takaniroi
Nitta Nariaki
Norton Aimee Ann
Nosé Masahito
Nosikov Igor

101
130
99
69
103
49
85, 128
87

O
Obridko Vladimir
Oinats Alexey
Okoh Daniel
Oleynik Philipp
Onwuneme S.E.
Ovodenko Vladimir
Owolabi Oluwafisayo Paul
Oyeyemi Elijah Oyedola

8, 9, 4267, 68
84
133
84
87
72
72, 84РPandya Megha
Panneerselvam C.
Parkhomov VladimirParnikov Stanislav
Pashinin Aleksandr
Patil P.
Pautet Pierre-Dominique
Pedlenton Jr. W.R.
Penskikh YuryPeters Dieter
Pereira Nuno
Perevalova Natalia
Perezhogin Andrey
Perminov Vladimir
Pevtsov Alexei
Piantschitsch Isabell
Pilipenko Vyacheslav
Pillai Ajesh Asokan
Pilipenko Vyacheslav
Pipin Valerii
Pirguliyev Mahir
Poddelsky Aleksey
Podgorny Alexander
Podgorny Igor
Podgórski Piotr
Podlesnyi Aleksey

10, 8566
1277, 8612, 100, 102
57
59
59
66
112
43, 47, 48, 123
62, 64, 65, 68
120
119
36
28
71, 80738030, 31, 50
20, 2191
4
4
19
68, 91, 95

Poedts Stefaan
Pogoreltsev Alexander
Polekh Nelya
Polozov Yury
Ponomarchuk Sergey
Potapov Alexander
Prech Lubomir
Prosovetsky Dmitry
Pustilnik Lev Aron
Pustovalova Lubov*PWING Team

21
107
96
77
91
29
16
17
18, 9037, 5678

Q
Qi JinQian Liying
Quémerais Eric

131
109
123

R
Rabiu Babatunde Akeem
Rakhmatulin Ravil
Rapp Markus
Russell III James
Ratnam Venkat
Ratovsky Konstantin
Redmon Robert
Reeves Geoffrey
Rodkin Denis
Romanova ElenaROSMIC WG3 Team
Rouanet Nicolas
Rowland William
Rozanov Eugene
Rudenko George
Rupesh Ghodpage
Ruzmaikin Alexander
Rybak Alexey

S
Sakharov Yaroslav
Salakhutdinova Irina
Samsonov Sergei
Samwel Susan
Sandeep Kumar
Sapronova Ludmila
142

72, 84100, 10259
112, 114
48
55, 56, 62, 64, 109
126
85
15
65
35
48
126
34
8, 9
35
46

71, 8014
71, 8017
10, 8566

Sarkissian Alain
Schmutz Werner
Sedykh Pavel
Semenov Anatoly
Semkova J.V.
Selivanov Vasiliy
Selvakumaran RavindranSetov Artem
Seredkin Ilya
Sergeev Viktor
Sergeeva Maria
Sezen Umut
Shapovalov Serge
Shagimuratov Irk
Shen Chenglong
Shepherd Gordon
Shepherd Marianna Genova
Shergelashvili Bidzina
Sherstyukov Roman
Shestakov Nikolay
Shevchuk Nikita
Shevtsov Boris
Shikhovtsev Artem
Shinbori Atsuki
Shiokawa Kazuo
Shiota Daikou
Shpynev Boris
Shugay Yulia
Siarkowski Marek
Simms Laura
Sivtseva Vera
Slemzin VladimirSluse Dominique
Smirnov Sergey
Smith Steve
Smolkov Gennady
Sokolova Zinaida
Soloviev Anatoly
Solovyev Igor
Somov Boris
Sormakov Dmitry
Sripathi Samireddypalle
Stefan Cristiana
Stepanov Alexander
Stepanov NikitaStęślicki Marek
Stober Gunter
Sukanta Sau
Sukhodolov Timofei
Sun Yan-Yi

123
123
81
63, 119, 1207680
1094, 95
120
100
83
135
121
97
6, 7
118
118, 124
21
67
62
107, 118
77, 120119
128
32, 78, 84
2260, 61, 116, 120
15
19, 23, 47
80
121
15
47
111
59
90
133
130
79, 12772574
41
5, 82, 89
100
47
59
57
107
52

Sunda Surendra
Suvorova Alla
Svinkin Dmitry
Sych Robert
Sylwester Barbara
Sylwester Janusz
Syrenova Tatyana

74
55
133
3
23
19, 2398

T
Tashlykov Viktor
Talpeanu Dana Camelia
Tan Baolin
Tanaka Yoshimasa
Tarun Kumar Pant
Taylor Michael John
Temmer Manuela
Tepenitsyna Nadezhda
Thiéblemont Rémi
Thithonis Maria Antonita
Timofeeva Olga
Tilton Margaret
Tkachev Ivan
Tlatov Andrey
Tlatova Kseniya
Toker Cenk
Tomikawa Yoshihiro
Tomozov Vladimir
Tolstikov Maxim
Toriumi Shin
Troshichev Oleg
Trushali Suresh Vasagade
Tsai-Lin Rung
Tsegmed Botulai
Tsepakina Irina
Tsinganos Kanaris
Tsurutani Bruce
Tsutsumi Masaki
Tsvetkova Anastasia

92, 94
15
29
128
73
59
102
97
123
60
64, 6512695
43
4354, 1236930
62
13
25, 101, 121
129
52
12, 29, 65
99
123
114
69
133

U
UeNo Satoru
Ulanov Mikhail
Umemura Norio
Uralov Arcadiy
Usoskin Ilya
Utchaikin Evgeniy

128
133
128
18, 21, 24
32
99

143

Uvarov Vladimir

V
Vail Chris
Valev Dimitar
Varlamov Ilya
Vasiliev Pavel
Vasilyev Roman
Vasil’eva Valeriya
Veenadhari Bhaskara
Verigin Mikhail
Veronig Astrid
Vidrenkova Anastasia
VineethChandrashekaharan Nair
Vlasova Natalia
Voeykov Sergey
Volodin Evgenii
Vršnak Bojan

W
Wang Jack Chieh
Wang Min
Ward William
Wang Yuming
Watanabe Takashi
Webb DaveWei Wang
Werner Rolf Heinz
West Matthew
Wimmer-Schweingruber
RobertWissing Maik
Wu QianX
Xie Hong

137

Y
Yakhnin Aleksandr
Yakimova Galina
Yan Yihua
Yankovsky Valentine
Yashiro Seiji
Yasyukevich Anna
Yasyukevich Yury

51
93, 95, 98, 134
4385
86, 87, 89
102
44
73

Yermolaev Michael
Yermolaev Yuri
Yigit Erdal
Yue Jia12
97
28, 29108
10, 24, 104
60, 61, 67, 109
67, 87, 93, 105,
109, 132
130
130
69
52

105
62
120
28, 102

Z
Zagainova Yuliya
Zaitsev Valery
Zakharenkova Irina
Zalyaev Timur
Zic Tomislav
Zimovets Ivan
Zhang Shunrong
Zhao Yucheng
Zhivetiev Ilya
Zhdanov Dmitry
Zherebtsov Geliy
Zolesi Bruno
Zolotukhina Nina
Zossi Bruno
Zossi Marta

8, 9, 11
5
55
77
28
12
104
59
67, 105
21
40, 68, 98
61
96
54, 55
38

124
113
82

52
3
124
6
127, 128103
28, 2985, 113
16
123
103
124

10

144

Second VarSITI General Symposium

ABSTRACTS

Editor-in-chief V.I. KurkinФормат 60×90 1/8. Гарнитура Times New Roman.
Усл. печ. л. 17.5. Уч.-изд. л. 21. Тираж 200. Заказ № 175 от 15 июня 2017 г.

Отпечатано в издательском отделе ИСЗФ СО РАН
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