Variability of the Sun and Its Terrestrial Impact (VarSITI)
SEE / ISEST-Minimax24 / SPeCIMEN / ROSMIC
http://www.varsiti.org/

Vol. 12, February 2017

Inside this issue
Article 1:
An introduction on ISEST(International Study of EarthAffecting Solar Transients)
Working Group on Theory………1
Article 2:
Database of global “EIT waves”
identified by the Coronal Pulse
Identification and Tracking Algorithm (CorPITA)………3
Article 3:
ULF Wave Power Index for theSpace Weather and Geophysical Applications………4
Highlight on Young Scientists 1:
Christina Kay / USA………7
Highlight on Young Scientists 2:
Daniela Wenzel / Germany………8
Highlight on Young Scientists 3:
David Pisa / Czech Republic………9
Meeting Report 1:
IAU Symposium 327: Fine Scale
Structure and Dynamics of the
Solar Atmosphere……10
Meeting Report 2:
ISEE Workshop on Ionosphericplasma bubble seeding anddevelopment……10
Upcoming Meetings……12

Project ISEST

VarSITI Newsletter
Article 1:

An introduction on ISEST (International Studyof Earth-Affecting Solar Transients) Working
Group on Theory
Bojan Vrsnak
Hvar Observatory, Croatia
Bojan VrsnakIn June 2013, a kick-off meeting of the
ISEST program (International Study ofEarth-Affecting Solar Transients) was
held at Hvar, Croatia (Figure 1),
following an initiative by Jie Zhang,
Yuming Wang, and Nat Gopalswamy.
This workshop, organized by Hvar
Observatory, was a kind of “forerunner”
of the forthcoming launch of the VarSITI/SCOSTEP program in January 2014.

activities. Beside plenary sessions, thework at the meeting was organized in fourgroups (WG1: Data, WG2: Theory, WG3:
Simulation, WG4: Event Campaign),
which became a backbone of the ISEST
program. Later on, three more groups
were added (WG5: Bs Challenge, WG6:
Solar Energetic Particles, WG7: MiniMax
Campaign).

T

he overall aim of WG2 is to advanceour comprehension of the physicalbackground of Earth-affecting solar
transients. The main goals can besummarized as follows:- to improve the understanding of thestructure and evolution of coronal massejections (CMEs) as well as their origin
and their magnetic structure, including the
problem of modelling the southwardmagnetic field component (Bs);- to improve comprehension of the
Figure 1. ISEST Kick-off meeting, coronal and heliospheric dynamics ofJune 17-20 2013, Hvar, Croatia (http:// CMEs, including the interaction withspaceweather.gmu.edu/meetings/
ambient solar wind and interplanetary
ISEST/Home.html).
magnetic field, causing deceleration/
The workshop was attended by 36 acceleration and deflections;participants from 14 countries (http:// - to get a better insight into how long
does the Lorentz force dominate over the
spaceweather.gmu.edu/meetings/ISEST/
Home.html). The main goal of the aerodynamic drag force, including theestimation of the drag parameter and/or
meeting was to formulate objectives ofthedimensionless drag coefficient;
the ISEST program and its further

VarSITI Newsletter・Vol. 12

- to compare the results derived by different analytic andnumerical models with observations, e.g., 1 AU transit
time, impact speed, impact magnetic field, etc.;- to advance understanding of the structure and evolutionof corotating interaction regions and physical relationshipwith coronal holes.

al. 2014) and Snow Plough Model (SPM; Tappin, 2006).
In recent years, the DBM started to be frequently
employed tool used to understand better various aspectsof the heliospheric dynamics of CMEs (e.g., Wang et al.
2016 and references therein). The CME deflected
propagation in the solar wind was reproduced in a 3D
MHD simulation (Shiota et al. 2016). Comparisons oft this point, the WG2 operational activity is mainly results based on analytical models and those based on
directed to advancing analytic CME-propagation numerical models have become another important aspectmodels that can be used for the forecasting purposes, of WG2 activity, such as ENLIL, COIN-TVD, CESE,
such as the Drag Based Model (DBM, Žic et al. 2015 and and H3DMHD (Figure 2; Vršnak et al. 2014).
references therein), the Deflection Model (DIPS; Wang etAFigure 2. Comparison of numerical ENLIL code and analytic Drag-Based Model (DBM).
a) ENLIL simulation (http://iswa.gsfc.nasa.gov/iswa/iSWA.html); b) DBM output (http://oh.geof.unizg.hr/
DBM/dbm.php). Snapshots show the situation on 2012 April 26 (12 UT and 07 UT for ENLIL and DBM,
respectively), representing the CME that was launched on 2012 April 23. c) DBM-calculated vs. ENLILcalculated Sun-1AU transit times for a sample of 50 CMEs (adopted from Vršnak et al. 2014).

References:
Möstl, C., Rollett, T., Frahm, R. A., et al.: 2015, Nature Communications, 6, 7135.
Shiota, D., Iju, T., Hayashi, K., et al.: 2016, AGU Fall Meeting, SH22B-03.
Tappin, S. J.: 2006, Solar Phys., 233, 233.
Vršnak, B., Žic, T., Temmer, M., et al.: 2014, ApJS, 213, 21.
Wang, Y., Wang, B., Shen, C., et al.: 2014, JGR, 119, 5117.
Wang, Y., Zhang, Q., Liu, J., et al.: 2016, JGR, 121, 7423.
Žic, T., Vršnak, B., Temmer, M.: 2015, ApJS, 218, 32.
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VarSITI Newsletter・Vol. 12

Project ISEST

Article ２:

Database of global “EIT waves” identified by the Coronal Pulse
Identification and Tracking Algorithm (CorPITA)David Long and David Pérez-Suárez
Mullard Space Science Laboratory,
University College London, UK

David Long“E

IT waves” are globally-propagating bright wavelike features associated with a solar eruption that
can traverse the solar disk in under an hour (see Figure1). They were first observed by SOHO/EIT in 1997
(e.g., Moses et al., 1997; Dere et al., 1997; Thompson etal., 1998) but are not yet fully understood. However,they are strongly associated with coronal mass ejections(CMEs) and could provide opportunities to study boththe solar corona through which they propagate (via coro-David Pérez-Suárez

nal seismology) and the associated CME itself. Although
they can be readily identified “by-eye” using moving
images, identifying and tracking them over an extended
period of time requires extensive image processing ofindividual images. This approach is complicated by thesheer volume of data provided by the Solar Dynamics
Observatory (SDO), which has necessitated development of automated techniques for identifying and tracking dynamic solar features (cf. Martens et al., 2012).

Figure 1. An “EIT wave” event observed on 12-May-1997 by the SOHO/EIT instrument. Theserunning difference images (wherein a following image is subtracted from a leading image) areused to highlight the moving pulse and make it easier to identify in single images.

T

he Coronal Pulse Identification and Tracking Algorithm (CorPITA; Long et al., 2014) was designed
to identify, track and analyse global “EIT waves” using
SDO images in the 211Å passband. The code is triggered by the start time of a solar flare, using its location
as a source and searching for any bright transient featureradiating from there. CorPITA uses a series of overlapping arc sectors to produce intensity profiles which are
examined to identify a moving pulse. If a pulse is detected, the algorithm tracks it for as long as possible
before measuring its velocity and acceleration in eacharc. The derived properties of the pulse are then used todetermine a quality rating, which defines the confidence
that the detection is a true “EIT wave” pulse. An example of the output provided by CorPITA is shown in Figure 2.

T

he process of putting the output from the CorPITA
code online has begun thanks to a grant awarded by
the VarSITI consortium. The grant was used to fund anundergraduate student who began running CorPITA
systematically by applying it to 238 “EIT wave” events
previously identified by Nitta et al. (2013). This is thefirst step in compiling a database of “EIT waves” andalso provides a benchmark for the effectiveness of thecode. The initial database is available online at https://sites.google.com/site/daithisolar/research/corpita, andwill be added to as more events are processed.

VarSITI Newsletter・Vol. 123Figure 2. An example of the output from CorPITA, in this case an event from 13-March-2012. The codeprovides a visual output of the identified pulse (left panel) and a plot of the fitted kinematics of the highest
rated arc sector (right panel).

Project SPeCIMEN

References:Dere, K. P., Brueckner, G. E., Howard, R. A., et al., 1997, Solar Physics, 175, 601.
Long, D. M., Bloomfield, D. S., Gallagher, P. T., & Pérez-Suárez, D., 2014, Solar Physics, 289, 3279.
Martens, P. C. H., Attrill, G. D. R., Davey, A. R., et al., 2012, Solar Physics, 275, 79.
Moses, D., Clette, F., Delaboudinière, J.-P., et al., 1997, Solar Physics, 175, 571.
Nitta, N. V., Schrijver, C. J., Title, A. M., & Liu, W., 2013, The Astrophysical Journal, 776, 58.
Thompson, B. J., Plunkett, S. P., Gurman, J. B., et al., 1998, Geophysical Research Letters, 25, 2465.

Article 3:

ULF Wave Power Index for Space Weather and GeophysicalApplications
V.A. Pilipenko(1,2) , O.V. Kozyreva3,
M.J. Engebretson4, and A.A. Soloviev(1,3)
1. Geophysical Center, Moscow, Russia
2. Space Research Institute,
Moscow, Russia
3. Institute of Physics of the Earth,
Moscow, Russia
4. Augsburg College, Minneapolis, USA

T

V. A. Pilipenko

he interaction between the solar wind (SW) andterrestrial magnetosphere is the primary driver ofthe processes occurring in the near-Earth environment.
This interaction has often been viewed using the implicit
assumption of a laminar plasma flow. Various geomagnetic indices and averaged SW/IMF parameters quantify
the energy supply in certain regions of the SW-

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VarSITI Newsletter・Vol. 12

O.V. Kozyreva

M.J.Engebretson A.A. Soloviev

magnetosphere-ionosphere system, and are used as primary tools in studies of solar-terrestrial relationships.
However, these indices characterize the steady-state level of the electrodynamics of the near-Earth environment.
The turbulent character of SW drivers and the existenceof natural MHD waveguides and resonators in the ULF
frequency range (~2-10 mHz) ensures a quasi-periodic

response to forcing at the boundary layers. We have elaborated a new index, coined a “ULF wave power index,”characterizing the turbulent character of the energy transfer from the SW into the upper atmosphere and the shortscale variability of near-Earth electromagnetic processes.

range 60o-75o. The output value has been normalized by
the spectral width to make the index dimension [nT].

Ground magnetic fluctuations are not always a perfectimage of ULF waves in the magnetosphere. Therefore, the ground global index needs to be augmented by a
ven a provisional version of the index has been suc- similar index, estimated from space magnetometer data.
cessfully used in various areas of space geophysics. This wave index, coined the GEO ULF-index, is calculatAn hourly ULF wave index, using the spectral features of ed from 1-min 3-component magnetic data from GOESULF power in the Pc5 band (periods from ~500 sec to satellites to quantify the ULF fluctuations and waves in~150 sec) is derived from a world-wide array of magne- the region of geostationary orbit. Additionally, to quantify
tometers in the Northern hemisphere.
the short-term variability of IMF and SW plasma, theinterplanetary ULF indices are estimated using 1-min dataor any UT hour, the magnetic stations in a chosen from the OMNI database.
MLT sector and in a selected CGM latitude range are
selected. The amplitude spectra F(f) of each horizontal
he hourly ULF index database has been compiled forcomponent are calculated in a 1 hour running window. A
the period since 1991 up to nowadays, and is permadiscrimination line, separating the background noise and nently updating. The database is freely available via thesignal spectra S(f), is determined as the linear fit in log- specially designed website http://ulf.gcras.ru/. The weblinear plot of F(f) (Figure 1). A spectral bump above the site provides a user the possibility:
to browse and download monthly plots and ASCII
discrimination line is considered as a contribution from afiles with basic space weather information, including
narrow-band signal.
the ground, geosynchronous, and interplanetary ULF
indices;
to browse and download daily plots with world-wide
magnetometers, GOES magnetometers, and basic
SW/IMF parameters;
Additionally, the website provides a list of downloadable
journal publications and conference talks related to theuse of ULF wave index in space weather studies.

E
F

T
●

●

A

wide range of space physics studies already benefited from the introduction of this new index. ULF
waves in the Pc5 band have emerged as a possible energy
reservoir (“geosynchrotron”) for resonant acceleration ofmagnetospheric electrons to relativistic energies. The introduced ULF wave index became a convenient tool in a
Figure 1. Schematic plot of the technique for thediscrimination of signal and noise from the power
correlative statistical studies of high-energy particle enerspectral density of ULF variations.
gization. The daily relativistic electron flux at geostationary orbit can be predicted with multiple regression analThe global ULF wave index is calculated from the 2.0-7.0 yses using a set of variables, including ground ULF andmHz band-integrated total power at each station. The sta- VLF wave powers. The combined effect of ULF and VLF
tion with a maximal amplitude is selected for each UT. waves shows a synergistic interaction, where each inFor the calculation of the provisional version of the creases the influence of the other on flux enhancement.
ground ULF index stations have been selected from The elaborated statistical models are able to predict (with
LT1=05 to LT 2=15 to suppress the contribution of accuracy ~80%) (Figure 2) increases of relativistic elecnighttime substorm activity, and in the CGM latitude tron fluxes at geosynchronous orbit.

Figure 2. A time plot of the observed (solid line) and predicted values with the one day lag model(dashed line) of electron flux at geosynchronous orbit from Simms et al. , JGR 2016.

VarSITI Newsletter・Vol. 125The level of upstream SW turbulence determines the firmed that when the SW is more turbulent, the effective
degree of the flow coupling with the magnetosphere. degree of its coupling to magnetosphere is higher, andUsing the ULF index of the IMF variability, it was con- the magnetosphere is driven more strongly (Figure 3).

Figure 3. Comparison of the auroral response, as characterized by hourly AE index, withthe strength of the SW driver, determined by the IMF Bz component, for the calm (log
SIMF<0, blue dots) and turbulent (log SIMF>0, red dots) IMF for the period 1994-1995 from
Romanova et al . , 2008.

ULF wave power in the SW was proposed to be an additional factor in controlling the coupling of the SW –magnetosphere - ionosphere system. Elevated ULF
wave power can substantially enhance the convection in
the high latitude ionosphere. The average cross polar cap
potentials show a roughly linear dependence on the ULF
interplanetary index. The variability of the SW might be
an important factor in triggering magnetospheric substorms. Application of statistical methods for the search

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VarSITI Newsletter・Vol. 12

for wave precursors of substorms will benefit from thedevelopment of an index quantifying ULF activity.

Awide range of space physics studies may benefit
from the introduction of the new hourly wave indices. Comments and requests for the ULF index construction are welcomed via website (http://ulf.gcras.ru/
feedback.html). This research was supported by a grantfrom SCOSTEP/VarSITI.

Predicting CME Deflections and Rotations andtheir Effect on the Magnetic Field of Near Earth
CMEs
Christina Kay
Solar Physics Lab, NASA Goddard Space Flight Center, USAoronal mass ejections (CMEs) often do not
propagate radially following an eruption. Single coronagraph observations show latitudinal deflections and multiple coronagraphs can be used toreconstruct longitudinal deflections (e.g. [1]). Observations and simulations also show that CMEs canrotate, changing their orientation with respect to thesolar equator. The largest deflections and rotations
occur in the corona, but interplanetary deflection canalso occur [2].

We developed a model, Forecasting a CME’s
Altered Trajectory (ForeCAT, [3]), to predictthe coronal deflection and rotation of CMEs using
the background magnetic pressure gradients andmagnetic tension. We have shown that ForeCAT

Figure 1: ForeCAT results for the 2010 April 8 CME,
which match the observed trajectory. The color contours show the magnetic field at the solar surface. Theline contours show the magnetic field farther out, withthe darkest lines indicating the location of the Heliospheric Current Sheet (HCS). The CME is initiatedparallel to the polarity inversion line of an active region. The CME deflects south along the HCS and therotation brings the CME orientation more parallel tothat of the nearby HCS.

matches the general trends in CME deflection androtation [3] and can reproduce individual observed
CMEs (e.g. [4]). Figure 1 shows a sample ForeCAT
simulation.

T

he presence of southward magnetic field is oneof the key drivers of geomagnetic storms, so
understanding a CME’s near-Earth magnetic field iscritical for accurate space weather predictions. ForeCAT determines the location and orientation of a
CME, which we use to simulate the passage of a flux
rope past a spacecraft in a new model, the ForeCATIn Situ Data Observer (FIDO, [5]). Figure 2 compares FIDO results with observations showing that
FIDO can reproduce a CME’s in situ magnetic fieldon large scales.

on Young Scientists

C

Christina Kay

Highlight

Project ISEST

Highlight on Young Scientists 1:

Figure 2: FIDO results for the 2010 May 24 CME. The
black and blue lines correspond respectively to the ACE andWind data and the red line shows the FIDO simulation.

References:
1. Xie, H., St. Cyr, O.C., Gopalswamy, N. et al. (2009), On the Origin, 3D Structure and Dynamic Evolution of CMEs Near Solar Minimum, Sol. Phys., 259: 143. doi:10.1007/s11207-009-9422-x.
2. Wang, Y., Wang, B., Shen, C., Shen, F., and Lugaz, N. (2014), Deflected propagation of a coronal massejection from the corona to interplanetary space, J. Geophys. Res. Space Physics, 119, 5117–5132,
doi:10.1002/2013JA019537.
3. Kay, C., Evans, R. M., and Opher, M. (2015), Global Trends of CME Deflections Based on CME andSolar Parameters, ApJ, 805, 168, doi:10.1088/0004-637X/805/2/168.
4. Kay, C., Opher, M., Colannino, R. C., and Voulidas, A. (2016), Using ForeCAT Deflections and Rotations to Constrain the Early Evolution of CMEs, ApJ, 827, 70, doi:10.3847/0004-637X/827/1/70.
5. Kay, C., Gopalswamy, N., Reinard, A., and Opher, M. (2017), Predicting the Magnetic Field of EarthImpacting CMEs, ApJ, 835, 117, doi: 10.3847/1538-4357/835/2/117.

VarSITI Newsletter・Vol. 127Highlight

Project ROSMIC

Highlight on Young Scientists 2:

VLF‑based Flare Detection
Daniela Wenzel
German Aerospace Center (DLR)
Institute of Communications and Navigation, GermanyI
on Young Scientists

n my PhD studies at the German Aerospace Center in Neustrelitz, I took part in the constructionof a ground based Global Ionospheric Flare Detection System (GIFDS). GIFDS is based on a globally
distributed network of Very Low Frequency (VLF)
receivers tuned to receive signals from Navy VLF
stations in order to continuously monitor the dayside lower ionosphere. Since X-ray flares cause anenhanced ionisation of the daytime D-region, corresponding VLF paths experience a related change
measured in the amplitude. In my analysis of flare
events from April 2014 to May 2015, the VLF amplitude was compared to the original solar X-ray

Daniela Wenzel

flux measured by GOES. The relative changes ofboth observations follow a trend shown in Fig. 1.

In order to confirm a flare activity, GIFDS iscombining multiple VLF signals by a weighted
arithmetic mean [1] . The weights depend on thesolar elevation at the path’s midpoint. Fig. 2
demonstrates a strong correlation of the resulting
superposition (top) and the GOES’ original X-ray
flux (bottom). With a resolution of 1 second GIFDS
is able to operate complementary to the wellestablished GOES system.

Figure 1: Relative VLF amplitude perturbations over the relative X-ray flux changeof solar flares derived from the VLF path
between HWU (France: 20.9 kHz) to
Neustrelitz.

Figure 2: Compound VLF measurement and the corresponding
solar X-ray flux measured by GOES.

Reference:[1] D. Wenzel, N. Jakowski, J. Berdermann, C. Mayer, C. Valladares, and B. Heber (2016), Global
ionosphericflare detection system (GIFDS). J. Atm. Sol.-Terr. Phys., 138-139, 233-242, doi: http://dx.doi.org/10.1016/j.jastp.2015.12.011.

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VarSITI Newsletter・Vol. 12

Langmuir and beam-mode waves upstream of the planetary bow shock
David Pisa
Institute of Atmospheric Physics
The Czech Academy of Sciences, Czech Republicn front of planetary magnetospheres the solar
wind flow slows down and forms a collisionless
bow shock. Solar wind electrons accelerated at theshock front are reflected back into the solar windforming electron beams. In regions containing theseelectron beams, foreshocks, Langmuir and beammode waves are typically observed (Fig. 1). In a
relatively narrow region behind the leading magnetic field line tangent to the bow shock, Langmuir
waves are most intense and observed as narrow
band emissions with single peak spectra at a frequency close to the electron plasma frequency [1,2]. Deeper downstream, waves are often more complex showing a wide frequency spread with upshift-

ed or downshifted emissions.

In our recent research, we focus on wave and particle analysis upstream of the terrestrial bow
shock as observed by the Cluster 2 spacecraft inyears from 2004 to 2010. Using an automated method, we have identified almost 7 x 105 spectra withintense wave emissions. Close to the upstream
boundary of the foreshock, the emissions are themost intense and at a frequency very close or above
the plasma frequency. Deeper downstream, thewave intensity is decreasing and the peak frequency
is shifting below the local electron plasma frequency.

on Young Scientists

I

David Pisa

Highlight

Project SPeCIMEN

Highlight on Young Scientists 3:

Figure 1: Example of CLUSTER 2 measurements in the vicinity of the terrestrial bow shock on 17 January 2009.
(Top) Time-frequency spectrogram of one electric component observed by the WHISPER instrument. Orange
arrows show bow shock crossings. Magnetosheath and foreshock visits are labeled by green and red bars, respectively. (Middle) The local electron density obtained from the WHISPER measurements. (Bottom) The total magnetic field calculated from the Fluxgate magnetometer.

References:[1] Píša, D., G. B. Hospodarsky, W. S. Kurth, O. Santolík, J. Souček, D. A. Gurnett, A. Masters, and M. E.
Hill (2015), Statistics of Langmuir wave amplitudes observed inside Saturn's foreshock by the Cassini
spacecraft, J. Geophys. Res. Space Physics, 120, doi:10.1002/2014JA020560.
[2] Píša, D., O. Santolík, G. B. Hospodarsky, W. S. Kurth, D. A. Gurnett, and J. Souček (2016), Spatial
distribution of Langmuir waves observed upstream of Saturn’s bow shock by Cassini, J. Geophys. Res.
Space Physics, 121, doi:10.1002/2016JA022912.

VarSITI Newsletter・Vol. 12

9Project ISEST

Meeting ReportT

Meeting Report 1:

IAU Symposium 327: Fine
Scale Structure and Dynamics
of the Solar Atmosphere,
Cartagena de Indias, Colombia,
9-14 October 2016

he main scientific goal of this symposium wasto discuss recent results on the processes shaping the structure of the solar atmosphere and driving
plasma eruptions and explosive events.

T

his symposium brought together researchers, inboth theory and observation. A total of 76 scientists and students (27 female / 49 male) from 19
countries participated in IAUS327. The VarSITI
program was a co-sponsor of the symposium andpartially supported the participation of students.

Santiago Vargas Dominguez
National Astronomical Observatory - National University ofColombia, Colombia
IAUS327 organizer
Santiago Vargas Dominguez

I

Project ROSMIC

AU Symposium 327 entitled Fine Structure andDynamics of the Solar Atmosphere was the first
IAU symposium held in Colombia and took place
immediate after the XV Latin American Regional
IAU Meeting (LARIM, 2-7 October 2016) and theFirst Workshop on Astronomy Beyond the Common
Senses for Accessibility and Inclusion (8 October2016). The venue was the University of Cartagena
located within the walled city of Cartagena deIndias.

Meeting Report 2:

ISEE Workshop on Ionosphericplasma bubble seeding and development, 29 November-02
December 2016
Hisao Takahashi
National Institute for Space
Research, Brazil
Hisao Takahashi

Figure 1. Group photo of participants.

ipants from 8 countries joined the meeting and discussed in the topics of observation and interpretation, new measurements and simulation models.
Through the round table discussions participants
pointed out importance of a coordinated ionosphericobservation along the geomagnetic equator and alsomodelling of plasma bubbles using more realistic
global atmospheric model. The workshop program
andabstractsareavailableat
http://
stdb2.stelab.nagoya-u.ac.jp/2016_bubble_ws/. Special edition of the Journal of Progress on Earth andPlanetary Science(SPEPS/PESP) is open for submission of papers. All of the scientists working on the
topic mentioned above are welcome, and the website to get information of submission is: http://
progearthplanetsci.org/index.html

During the period from November 29 to December 02, 2016, “Workshop on Ionospheric plasma bubble seeding and development” has been heldat Institute for Space and Earth Environment Research (ISEE), Nagoya University, Nagoya, Japan.
It was supported by ISEE program of “Project for
Solar-Terrestrial Environment Prediction(PSTEP)”.
The main purpose of the meeting was to review today´s scientific understanding in the Equatorial plasma bubbles (EPBs) and to seek next steps. 23 partic-

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VarSITI Newsletter・Vol. 12

Figure 1. Group photo of participants.

Upcoming meetings related to VarSITI
Conference

Date

LocationContact Information

Data Analysis Workshop on
Coronal and Interplanetary Shocks: Data Analysis
from SOHO, Wind, and e-CALLISTO Data

Feb. 19-25, 2017

Mekelle, Ethiopia

http://www.mu.edu.et/cncs/
index.php/2/220-internationaldata-analysis-workshop-oncoronal-mass-ejections-ad-solarradio-bursts-coronal-andinterplanetary-shocks

The 10 years of operation of High resolution Neutron Monitor Database-NMDB

Mar. 20-23, 2017

Athens, Greece

http://cosray.phys.uoa.gr/
index.php/workshops2/10-yearsnmdb

EGU General Assembly

Apr. 23-28, 2017

Vienna, Austria

http://www.egu2017.eu/2017 International Conference on Space Science
and Communication

May 3-5, 2017

Kuala Lumpur,
Malaysia

http://www.ukm.my/iconspace/

JPGU-AGU Joint Meeting 2017

May 20-25, 2017

Makuhari, Japan http://www.jpgu.org/

the Ninth Workshop "Solar Influences on the Mag- May 30-June 3,
netosphere, Ionosphere and Atmosphere"
2017

Sunny beach,
Bulgaria

http://ws-sozopol.stil.bas.bg/

Advanced Concepts in Solar-Terrestrial Coupling in
the Context of Space Weather
July 9-14, 2017
A Concepts and Tools School for Students during
the VarSITI 2017 General Symposium

Irkutsk, Russia

http://en.iszf.irk.ru/
Space_weather_summer_school_2017

2nd VarSITI General Symposium

July 10-15, 2017

Irkutsk, Russia

http://varsiti2017.iszf.irk.ru

IAU Symposium 335 “Space Weather of the
Heliosphere: Processes and Forecasts”

July 17-21, 2017

Devon, UK

http://www.exeter.ac.uk/iaus335

AOGS 14th Annual Meeting

Aug. 6-11, 2017

Singapore

http://www.asiaoceania.org

URSI General Assembly and Scientific Symposium

Aug. 19-26, 2017

Montreal,
Canadahttp://www.ursi2017.org

IAPSO-IAMAS-IAGA Joint AssemblyAug. 27-Sep. 1,2017

Cape Town,
South Africa

http://www.iapso-jamasiaga2017.com

Consistency of the Solar Radius: outstanding unsolved points (ISSI Forum)

1st semester of2017

Switzerland

13th International Workshop on Layered PhenomSept. 18-22, 2017ena in the Mesopause Region (LPMR)

Kühlungsborn,
Germany

International Study of Earth-affecting Solar TransiSep. 18 – 22, 2017ents (ISEST/MiniMax24) Workshop in 2017

Jeju Island, Korea

AGU Chapman Conference, “Particle Dynamics inthe Earth's Radiation Belts”

Sept. 25-29, 2017

Biarritz, France

SCOSTEP 14th Quadrennial Solar-Terrestrial
Physics Symposium

July 9-13, 2018

Vancouver,
Canadahttps://www.iap-kborn.de/1/
current-issues/events/lpmr/

http://www.yorku.ca/scostep

VarSITI Newsletter・Vol. 1211The purpose of the VarSITI newsletter is to promote communication among scientists related to the four VarSITI Projects (SEE,
ISEST/MiniMax24, SPeCIMEN, and ROSMIC).
The editors would like to ask you to submit the following articles to the VarSITI newsletter.
Our newsletter has five categories of the articles:
1. Articles— Each article has a maximum of 500 words length and four figures/photos (at least two figures/photos).
With the writer’s approval, the small face photo will be also added.
On campaign, ground observations, satellite observations, modeling, etc.
2. Meeting reports—Each meeting report has a maximum of 150 words length and one photo from the meeting.
With the writer’s approval, the small face photo will be also added.
On workshop/conference/ symposium report related to VarSITI
3. Highlights on young scientists— Each highlight has a maximum of 200 words length and two figures.
With the writer’s approval, the small face photo will be also added.
On the young scientist’s own work related to VarSITI
4. Short news— Each short news has a maximum of 100 words length.
Announcements of campaign, workshop, etc.
5. Meeting schedule
Category 3 (Highlights on young scientists) helps both young scientists and VarSITI members to know each other. Please contact the editors if you know any recommended young scientists who are willing to write an article on this category.
TO SUBMIT AN ARTICLE
Articles/figures/photos can be emailed to the Newsletter Secretary, Ms. Megumi Nakamura (nakamura.megumi_at_isee.nagoyau.ac.jp). If you have any questions or problem, please do not hesitate to ask us.
SUBSCRIPTION - VarSITI MAILING LISTThe PDF version of the VarSITI Newsletter is distributed through the VarSITI mailing list. The mailing list is created for eachof the four Projects with an integrated list for all Projects. If you want to be included in the mailing list to receive future information of VarSITI, please send e-mail to “nakamura.megumi_at_isee.nagoya-u.ac.jp” (replace “_at_” by “@”) with your full
name, country, e-mail address to be included, and the name of the Project you are interested.

Kazuo Shiokawa (shiokawa_at_isee.nagoya-u.ac.jp)
Center for International Collaborative Research (CICR),
Institute for Space-Earth Environmental Research (ISEE), Nagoya University,
Nagoya, Japan
Tel: +81-52-747-6419, Fax: +81-52-747-6323

Editors:

Katya Georgieva (kgeorg_at_bas.bg)
Space Research and Technologies Institute, Bulgarian Academy of Sciences,
Sofia, Bulgaria
Tel: +359-2-979-23-28
Newsletter Secretary:

Megumi Nakamura (nakamura.megumi_at_isee.nagoya-u.ac.jp)
Center for International Collaborative Research (CICR),
Institute for Space-Earth Environmental Research (ISEE), Nagoya University,
Nagoya, Japan
Tel: +81-52-747-6417, Fax: +81-52-747-6323

VarSITI Project co-leaders:

Piet Martens (SEE), Dibyendu Nandi (SEE), Vladimir Obridko (SEE), Nat Gopalswamy(ISEST/Minimax24), Manuela Temmer (ISEST/Minimax24), Jie Zhang (ISEST/
Minimax24), Jacob Bortnik (SPeCIMEN), Craig Rodger (SPeCIMEN), Shri Kanekal(SPeCIMEN), Yoshizumi Miyoshi (SPeCIMEN), Franz-Josef Lübken (ROSMIC),
Annika Seppälä (ROSMIC), and William Ward (ROSMIC)

SCOSTEP Bureau:

Nat Gopalswamy (President), Franz-Josef Lübken (Vice President), Marianna Shepherd(Scientific Secretary), Vladimir Kuznetsov (IUGG/IAGA), Mark Lester (IUPAP),
Takuji Nakamura (COSPAR), Annika Seppälä (SCAR), Craig Rodger (URSI),
Dan Marsh (IAMAS), and Kyung-suk Cho (IAU)
website: www.yorku.ca/scostep

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VarSITI Newsletter・Vol. 12