SCOSTEP/PRESTONEWSLETTER
Vol. 30, January 2022

Inside this issue
Article 1:
The Dimmest Stateof the Sun

1

Article 2:
Ionospheric Equatorial Scintillation inSouthern Crest over
Kinshasa (DRC)

35Highlight onYoung Scientists 1:
Subir Mandal / India
Highlight onYoung Scientists 2:
Satabdwa Majumdar / India

Article 1:

The Dimmest State of the Sun

Kok Leng Yeo1
1Max Planck Institute for Solar System Research,Göttingen, GermanyH

ow the amount of solar electromagnetic radiation entering the Earthsystem, described in terms of Total Solar
Irradiance (TSI), varied since pre-Kok Leng Yeo

industrial times is an important consideration in the climate change assessment.
The industrial revolution is preceded by
the Maunder minimum, an extended peri-

68
Meeting Report 1:
The Hinode-14/IRIS11 Joint Science
Meeting
Meeting Report 2:
The International
Space Weather Initiative (ISWI) Workshop

8

Upcoming Meetings

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Figure 1. A) Solar activity since the Maunder minimum as indicated by the groupsunspot number (black: Hoyt and Schatten 1998; red: Svalgaard and Schatten 2016).
B) The reconstruction of TSI over the same period from the SATIRE-T (Wu et al.,2018, black), NRL (Coddington et al., 2016, blue) and CHRONOS models (Egorova
et al., 2018, red). C) The reconstruction of TSI since 2010 from SATIRE-3D (blackYeo et al., 2020) and the measurements from SORCE/TIM (Kopp et al., 2005, red).
We established, with this model, that the TSI level of the Sun in its least-active stateis 2.0±0.7 Wm−2 below the 2019 level, indicated by the shaded range.

SCOSTEP/PRESTO NewsletterVol. 30

Article
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2

Figure 2. Three-dimensional magnetohydrodynamics simulations of the solar surface and atmosphere. A)
Magnetic flux density at the solar surface in a snapshot of each simulation run and B) the corresponding
bolometric image, calculated using a radiative transfer code. The simulation runs were set up to emulate the smallscale turbulent dynamo. Three of the four runs were initiated with a uniform vertical magnetic field of 100, 200,
and 300 G, producing the magnetic aggregations in the intergranular lanes. The white box in the left column
denotes 1×1 arcsec, corresponding to an area of approximately 725×725 km on the Sun.

od of weak solar activity (Fig. 1A). Detrimental to theclimate change debate, current estimates of the rise in
TSI since the MM differ markedly, ranging from 0.1
Wm−2 to 6 Wm−2 (Fig. 1B). This is one of the reasons
why the exact contribution by solar forcing to the rise inglobal temperatures over the past centuries remains controversial. To address this issue, we adopted a novel
approach, based on state-of-the-art solar imagery andnumerical models, to establish the TSI level of the Sun
in its least active state (Yeo et al., 2020). Since this corresponds to the dimmest the Sun can be during grandactivity minima such as the MM, the difference to thepresent level represents the greatest possible rise in TSI
since the MM.

T

his work built on the groundbreaking model of TSI
variability presented by Yeo et al. (2017), SATIRE3D. Models of solar irradiance variability account for
the effect of solar surface magnetism on the brightnessof the Sun. For simplicity, other models estimate thiseffect from plane-parallel approximations of the heterogeneous solar atmosphere or, even more crudely, fromthe linear regression of indices of solar magnetism tosolar irradiance observations. Such approaches cannot
capture the relevant physics fully, with the result thatthese models require calibration to measured solar irradiance variability. SATIRE-3D employs realistic threedimensional models of the solar atmosphere (Fig. 2)
generated with a state-of-the-art magnetohydrodynamic(MHD) code (MURaM, Vögler et al., 2005). By establishing how these model solar atmospheres would appear to the HMI solar telescope onboard SDO (Scherrer
et al., 2012), SATIRE-3D is able to reproduce TSI variability from HMI observations while not requiring any
calibration to measured TSI variability (Fig. 1C), andremains the only reported model to achieve such a feat.

T

aking into consideration the dearth of sunspots during the MM (Fig. 1A), the timescale of stellar evolution and the findings of recent studies into the small-

SCOSTEP/PRESTO NewsletterVol. 30

scale turbulent magnetic field on the solar surface, we
argued the least active state of the Sun is where theglobal dynamo is dormant and the entire solar surface
resembles the present-day internetwork. (The internetwork refers to the solar surface outside of sunspots, faculae and network.) By incorporating newly-available
realistic MHD simulations of the internetwork into
SATIRE-3D, we established the TSI level of the least
active Sun to be 2.0±0.7 Wm−2 below the 2019 minimum level (Fig. 1C). This upper limit on the rise in TSI
since the MM, only one-third of the existing cap of 6.0
Wm−2, greatly restricts the possible role of solar forcing
in global warming.
References:
Coddington, O., Lean, J. L., Pilewskie, P., Snow, M.,
and Lindholm, D. (2016). A Solar Irradiance Climate
Data Record. Bull. A m. Meteorol. Soc., 97(7):1265.
Egorova, T., Schmutz, W., Rozanov, E., Shapiro, A. I.,
Usoskin, I., Beer, J., Tagirov, R. V., and Peter, T.
(2018). Revised historical solar irradiance forcing. A stron. Astrophys., 615:A85.

Hoyt, D. V. and Schatten, K. H. (1998). Group Sunspot
Numbers: A New Solar Activity Reconstruction. Sol.
Phys., 181(2):491–512.
Kopp, G., Lawrence, G., and Rottman, G. (2005). The
Total Irradiance Monitor (TIM): Science Results. Sol.
Phys., 230(1-2):129–139.
Scherrer, P. H., Schou, J., Bush, R. I., Kosovichev, A.
G., Bogart, R. S., Hoeksema, J. T., Liu, Y., Duvall, T.
L., Zhao, J., Title, A. M., Schrijver, C. J., Tarbell, T. D.,
and Tomczyk, S. (2012). The Helioseismic and Magnetic Imager (HMI) Investigation for the Solar Dynamics
Observatory (SDO). Sol. Phys., 275(1-2):207–227.
Svalgaard, L. and Schatten, K. H. (2016). Reconstruction of the Sunspot Group Number: The Backbone

620:A120.

Vögler, A., Shelyag, S., Schüssler, M., Cattaneo, F.,
Emonet, T., and Linde, T. (2005). Simulations of magneto-convection in the solar photosphere. Equations,
methods, and results of the MURaM code. A stron. A strophys., 429:335– 351.

Yeo, K. L., Solanki, S. K., Krivova, N. A., Rempel, M.,
Anusha, L. S., Shapiro, A. I., Tagirov, R. V., and Witzke, V. (2020). The Dimmest State of the Sun. Geophys.
Res. Lett., 47(19):e90243.
Yeo, K. L., Solanki, S. K., Norris, C. M., Beeck, B.,
Unruh, Y. C., and Krivova, N. A. (2017). Solar Irradiance Variability is Caused by the Magnetic Activity on
the Solar Surface. Phys. Rev. Lett., 119:9.1102.

Highlight on Young Scientists

Wu, C. J., Krivova, N. A., Solanki, S. K., and Usoskin,
I. G. (2018). Solar total and spectral irradiance reconstruction over the last 9000 years. A stron. A strophys.,

ArticleMethod. Sol. Phys., 291(9-10):2653–2684.

Article 2:

Ionospheric Equatorial Scintillation in Southern Crest over
Kinshasa (DRC)

Bruno Kahindo Murumba1
1University of Kinshasa, Kinshasa, Congohe Equatorial ionosphere is the turbulent fluctuations of electronic density that cause rapid variations ionosphere refraction index. The ionospheric scintillation is amplitude and phase perturbation of radio
signals up to 12 Ghz [ITU-R, 2012] traversing thesevariations. The data used come from the GPS SCINDA
Kinshasa site obtained from May 2011 to October 2012.

Stion 23°S including Kinshasa with 4.41°S, 15.30°E The
F-layer equatorial irregularities is vital for the designand operation of satellite communication systems affected up to microwave bands.

T

he Vtec is solar flux dependent, during thenighttime Vtec values are below 20 tecu. During
the day time, two equinoxes maximum for 80 tecu at 14
TU are coding from red to black colors. The first maximum of solar activity cycle 24 in November 2011 thesecond maximum stronger than the first in the beginningof 2012.The weakest period is in summer solstice with
about 35-45 tecu. The Tec symmetry of seasonal behavior relatively to the magnetic equator was shown. The
blue code means nighttime not affected by solar flux
almost 22.00 to 10.00 (Fig.1).

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tudies of ionospheric scintillations at equatorial latitudes reveal the existence of an intense belt of ionospheric irregularities in the night time F-region coveredby about ± 20º magnetic latitudes around the magnetic
equator include where the electrojet current controls
equatorial anomaly in the F2 region and the region of
the strongest ionization encompassing southern crest ofequatorial anomaly (~20°-25°S) with Magnetic inclina-

Meeting Report

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Bruno Kahindo
MurumbaAnnouncement

Figure 1. Three-dimensional VTEC Diurnal variation at DRC, 2012 (TEC Unit:1tecu=10 16 electrons / m2)(Kahindo et al.2017).

SCOSTEP/PRESTO NewsletterVol. 303Article
Highlight on Young Scientists
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Figure 2. Scintillations of Scinda GPS Kinshasa (2011-2012) [Kahindo et al, 2017].

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4T

he development of high amplitude scintillations was(S4 > 1.0) after 18UT (19.00 LT) and maximum
during the equinoxes but few scintillations in solstices(Fig. 2). The interest of these observations is occurringin the southern crest of equatorial anomaly where arevery few measurements.

Kahindo Murumba B., Kazadi Mukenga Bantu A., Fleury R., Tondozi Keto F., Zana Ndontoni A., Kakule Kaniki M., Amory-Mazaudier C., Groves K. (2017) : Contribution à l’étude de la scintillation ionosphérique équatoriale sur la crête sud de l’Afrique, Journal des Sciences, Vol. 17, N° 2, 27-47pp, I.S.S.N 0851 – 4631.

References:

Maruyama Takashi (2002): Ionosphere and Thermosphere: ionospheric irregularities, Journal of the Communications Research Laboratory Vol.49 No.3, doi:
10.1016/B978-0-12-821366-7.00003-2.

Amory-Mazaudier, C., Fleury, R., Petitdidier, M., Soula, S., Masson, F., GIRGEA team, Davila, J., Doherty,
P., Elias, A.G., Gadimova, S. ,Makela, J., Nava,
B.,Radicella, S.2, Richardson, J., Touzani, A.(2017) :Recent Advances in Atmospheric, Solar-Terrestrial
Physics and Space Weather from a North-South networkof scientists [2006-2016], Part B: Results and Capacity
Building, , Sun and Geosphere, International Journal of
Research and Applications, ISSN 2367-8852, vol.12, ,pp-21-69.p2df, BBC SWS Regional Network.

SCOSTEP/PRESTO NewsletterVol. 30

Richmond, A.D (1973): Equatorial electrojet, I, Development of a model including winds andinstabilities, J. Atmos. Terr. Phys., 35, 1083-1103,
doi:10.1016/0021-9169(73)90007-X.
Rishbeth, H. (1977): Dynamics of the equatorial F region, J. Atmos. Terr. Phys., 39, 1159-1168, DOI:
10.1016/0021-9169(77)90024-1.

Article

Highlight on Young Scientists 1:

Evidence of high-to-low latitude coupling in the daytime
thermopheric gravity wave activity during geomagnetically disturbed periods

M

Subir Mandal

analyses over a two-year duration from Ahmedabad,
India, showed that the vertical propagations of GWs in
the daytime thermosphere exist only 40% of the time
and they are strongly influenced by the solar flux variability (Mandal et al., 2020). During geomagneticallyquiet times, we found a double-humped structure in themagnitudes of vertical phase speeds (Cz) of these upward propagating GWs with maxima during equinoxes
and minima during solstices (figure-1a). Further, they

Meeting Reporty research is focused on understanding the effects of solar and geomagnetic forcing on thevertical propagations of gravity waves (GWs) over the
low-and-equatorial latitudes. We have arrived at a new
approach to derive vertical propagation characteristics(time periods, speeds, wavelengths) of GWs by monitoring the phase-offsets in height variations of multiple
iso-electron density contours as obtained using
digisonde measurements (Mandal et al., 2019). Such

Highlight on Young Scientists

Subir Mandal1
1Physical Research Laboratory, Ahmedabad, Gujarat, India

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Figure 1. (a) Seasonal variation in the vertical phase speeds of GWs for geomagnetically quiet days (blue triangles)
and HWM-14 model-derived winds (green curve). Monthly averaged values of C z (red diamonds) and the leastsquare fit (dashed curve) of these are shown. (b) Periodograms obtained from the Lomb-Scargle analyses of winds(green) and GW speeds (blue) are depicted, which show a nearly similar periodicity in them which is anticorrelated with their temporal behavior shown in (a). (c) Disturbed time vertical phase speeds of GWs (redtriangles) along with the quiet time average behavior (dashed curve). (d) Changes in C zvalues (red triangles)
during disturbed times compared to quiet days, and the integrated values of the AE index (blue asterisks) are
shown as a function of day of the year.

5Article
Highlight on Young Scientists

show anti-correlation and similar periodic variation withthe thermospheric model winds (figure-1b), suggestinga strong influence of background winds on wave propagations (Mandal and Pallamraju, 2020). The verticalpropagation speeds of GWs on geomagnetically disturbed days are found to be significantly different fromthe average quiet time behavior (figure-1c), represented
by least-square curve fitting. These differences in thevertical phase speeds (< Cz >d) for geomagnetically disturbed days have been found to show variation similar
to those in the integrated values of the auroral electrojet(AE) index, which is a measure of Joule heating in theauroral region due to energetic particle participations.
We propose that these changes in the propagation
speeds of GWs are brought in by the equatorward winds
generated due to heating in the high latitudes and hence,
present an evidence of high-to-low latitude coupling.

Mandal, S., Pallamraju, D., and Suryawanshi, P. (2020).
Changes in the daytime thermospheric gravity wave
propagation characteristics over low-latitudes in response to the variation in solar flux. Journal of Atmospheric and Solar-Terrestrial Physics,
https://
doi.org/10.1016/j.jastp.2020.105414.
Mandal, S., and Pallamraju, D. (2020). Thermosphericgravity wave characteristics in the daytime over lowlatitudes during geomagnetic quiet and disturbed conditions. Journal of Atmospheric and Solar-Terrestrial
Physics, https://doi.org/10.1016/j.jastp.2020.105470.

References:
Mandal, S., Pallamraju, D., Karan, D. K., Phadke, K.
A., Singh, R. P., and Suryawanshi, P. (2019). On deriving gravity wave characteristics in the daytime upper

Meeting Report
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atmosphere using radio technique. Journal of Geophysical Research: Space Physics, 124, 6985–6997. https://doi.org/10.1029/2019JA026723.

Highlight on Young Scientists 2:

Insights from the study of 3D evolution of CMEs
in inner and outer corona

Satabdwa Majumdar1
1Indian Institute of Astrophysics, Bengaluru, Karnataka, India

D

Satabdwa
Majumdarespite studying Coronal Mass Ejections (CMEs)
for the past few decades, the major challenges
faced are projection effects, and paucity of data in the
inner corona (< 3R). As a consequence of the later, Extreme UltraViolet observations are seldom combinedwith white light observations but unfortunately at thecost of questioning the consistency in the tracked physical feature.

evidence in support of a width acceleration equivalence
as nothing but a veritable manifestation of the same
Lorentz force. We further noted these two heights forseveral events and found that the distribution of theseheights (Figure 1(b)) are largely overlapping, with both
distributions peaking at 2.5 - 3 R. Thus further assertingthat the imprint of Lorentz force statistically stays dominant till 2.5-3R.

TA

hus, in Majumdar et al. (2020), we studied the 3D
kinematics of 59 CMEs in inner and outer coronaby implementing the Graduated Cylindrical Shell (GCS)
model (Thernesien et al. 2009) to the combined observations of COR-1 and COR-2 on-board the twin spacecraft STEREO-A/B.

In Figure 1(a) we see a complete kinematic profile ofa CME. In the third and fourth panel, we mark theheights of ceasing initial impulsive acceleration andrapid width expansion and find the two heights to lie
close to each other. Thus providing the observational

SCOSTEP/PRESTO NewsletterVol. 30s an extension, in Majumdar et al. (2021), we
found that the correlation of peak 3D speed andacceleration is different for CMEs originating from active regions (ARs) than those from quiescent and active
prominences (PEs and APs) (Figure 2(a) and (b)). Further, the correlation between average acceleration andaverage speed (Figure 2(c)) showed that the drag experienced by CMEs are also different for different
sources. Thus these results hint towards the possibilityof different ejection and propagation mechanisms for
CMEs connected to these different sources.

Article
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Figure 1. (a) A complete kinematic profile of a CME. The height time data is fitted with a smooth spline (in red)and the speed and acceleration profiles (with an inset for a zoom in to the residual acceleration phase) are plottedby taking and first and second order derivative of the height-time data and the spline fit to it. The fourth panel
shows the evolution of the half-angle parameter of the GCS model that communicates the angular width expansionof the CME. The blue vertical line (in third and fourth panel) markes the height at which the impulsive acceration
and rapid angular width expansion ceases. (b) The distribution of heights of ceasing impulsive acceleration andwidth saturation.

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References:
Majumdar, S., Pant, V., Patel, R., & Banerjee, D.
2020,388ApJ, 899, 6, doi: 10.3847/1538-4357/aba1f2.

Announcement

Figure 2. (a) Plot of peak acceleration versus peak speed. (b) Plot of the mean constant acceleration versus mean
speed in inner corona. The data points are color coded with respect to the source region they are coming from, andthe corresponding correlation coefficients are shown. The dashed line is the fitted emperial profile to the data.

Majumdar, S., Patel, R., Pant, V., & Banerjee, D.
2021b,390ApJ, 919, 115, doi: 10.3847/1538-4357/
ac1592.

Thernisien, A., Vourlidas, A., & Howard, R. A. 2009,
SoPh,441256, 111, doi: 10.1007/s11207-009-9346-5.

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Article

Meeting Report 1:

The Hinode-14/IRIS-11
Joint Science Meeting

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Meeting Report
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8

Figure 1. The logo of the Hinode-14/IRIS-11 Joint Science Meeting.

Jie Zhang1
1George Mason University,
Fairfax, VA, USA

Jie ZhangT

he Hinode-14 / IRIS-11 Joint Science meeting took
place virtually on October 25-29, 2021 and washosted by George Mason University (Fairfax, VA,
USA). The meeting highlighted the most recent
achievements of the IRIS and Hinode missions together
with the latest research on topics related to the missions’ goals. The science program was organizedaround four themes: (1) Hinode/IRIS connection to inner heliospheric platforms (PSP, SolO and other instru-

Meeting Report 2:

The International Space
Weather Initiative (ISWI)
Workshop
Tarun Kumar Pant1 and Sharafat
Gadimova2
1Space Physics Laboratory, Vikram
Sarabhai Space Centre, Thiruvananthapuram, India
2United Nations Office for Outer
Space Affairs (UNOOSA), Vienna,
Austria

Tarun Kumar
Pant

T

he 2021 online International Space Weather Initiative workshop on 'Space Weather: Science & Applications' was jointly organized on November 2-3,2021 by UNOOSA and the Space Physics Laboratory,
Vikram Sarabhai Space Centre (VSSC), of the IndianSpace Research Organization (ISRO), India. The Workshop was supported by International Committee on
Global Navigation Satellites (ICG), Boston College,
National Aeronautics and Space Administration(NASA), and Scientific Committee on Solar Terrestrial

SCOSTEP/PRESTO NewsletterVol. 30

metnts), (2) photospheric convection and solar magnetic
field, (3) atmospheric heating: chromosphere to coronaand (4) Flares, jets, CMEs and others. The fifth day was
dedicated to a tutorial to the usage of data from EIS,XRT and SOT, and SunPy and IRISpy software packages.

There were 350 registrations from 26 countries.
There were 138 abstracts submitted, distributing in
50 oral presentations (14 invited) and 88 posters. The
meeting acknowledges support from GMU, NSO, NSF,
NASA and SCOSTEP/PRESTO. The full meeting information can be accessed at http://hinode14.org.

Physics (SCOSTEP). Over 340 participants from 52
different countries attended the workshop. The faculties
comprised both national and International experts on
Sun, Space Weather, its science and applications. Various important aspects of the "Space Weather: Scienceand Application" were discussed in four sessions, titledas (1) Sun, Solar Wind and Extreme Solar Eruptions,(2) Space Weather - Sources, Consequences, Observations and Modeling, (3) Space Weather Impacts on
Magnetosphere - Thermosphere - Ionosphere System,and (4) Space Weather Instrumentation, Data, Outreachand Education.

T

he talks addressing topics concerning solar exploration, new payloads and probes, new and ongoingsolar missions provided a modern perspective to theparticipants. The workshop also familiarised the participants with available data resources. The participantsalso got exposed to the new niche and emerging areasof solar - terrestrial science and modelling thereof. In
addition, this workshop has been an important prelude
to the forthcoming 15th Quadrennial Solar Terrestrial
Physics Symposium, under the aegis of SCOSTEP, in
India in February, 2022. This initiative is planned tocontinue in future too.

A

ll the details and open-access lectures can be foundat the web-site: http://www.unoosa.org/oosa/en/
ourwork/psa/schedule/2021/2021-iswi-workshop.html.

Upcoming meetings related to SCOSTEPArticleDate

LocationContact Information

SCOSTEP’s 15th Quadrennial SolarTerrestrial Physics Symposium (STP-15)

Feb. 21-25, 2022

Onlinehttps://stp15.in/

EGU General Assembly 2022

Apr. 3-8, 2022

Vienna, Austria

https://www.egu22.eu/

The Second Summer School on Space Research, Technology and Application

Jul. 3-10, 2022

Rozhen, Bulgaria

https://bulgarianspace.online/
second-summer-school_2022/

COSPAR 2022

Jul. 16-24, 2022

Athens, Greece

http://
www.cosparathens2022.org/

AOGS 2022

Aug. 1-5, 2022

Onlinehttps://www.asiaoceania.org/
society/public.asp?
page=home.asp

Highlight on Young Scientists

Conference

16th International Symposium on Equatorial
Sept. 12-16, 2022 Kyoto, Japan
Aeronomy (ISEA-16)
In October, 2022

Houphouët Boigny
University, Abidjan, Côte d’Ivoire

AGU Fall Meeting 2022

Dec. 12-16, 2022

Chicago, IL, USA

https://www.agu.org/fall-meeting

IUGG 2023

Jul. 11-20, 2023

Berlin, Germany

https://www.iugg2023berlin.org/

AGU Fall Meeting 2023

Dec. 11-15, 2023

San Francisco, CA,USA

https://www.agu.org/fall-meeting

Meeting Report

Summer Space Weather School- Physics and use of tools

Please send the information of upcoming meetings to the newsletter editors.

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SCOSTEP/PRESTO NewsletterVol. 30

9

The purpose of the The purpose of the SCOSTEP/PRESTO newsletter is to promote communication among scientists related to solar-terrestrial
physics and the SCOSTEP’s PRESTO program.
The editors would like to ask you to submit the following articles to the SCOSTEP/PRESTO 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 SCOSTEP/PRESTO
3. Highlights on young scientists— Each highlight has a maximum of 300 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 SCOSTEP/PRESTO
4. Announcement— Each announcement has a maximum of 200 words length.
Announcements of campaign, workshop, etc.

5. Meeting schedule
Category 3 (Highlights on young scientists) helps both young scientists and SCOSTEP/PRESTO 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. Mai Asakura (asakura_at_isee.nagoya-u.ac.jp). If you have any questions or problem, please do not hesitate to ask us.
SUBSCRIPTION - SCOSTEP MAILING LISTThe PDF version of the SCOSTEP/PRESTO Newsletter is distributed through the SCOSTEP-all mailing list. If you want to be included in themailing list to receive future information of SCOSTEP/PRESTO, please send e-mail to “patricia.doherty_at_bc.edu” or “sean.oconnell.2 atbc.edu” (replace “_at_” by “@”) with your name, affiliation, and topic of interest to be included.

Editors:

Kazuo Shiokawa (shiokawa_at_nagoya-u.jp)
SCOSTEP President,
Center for International Collaborative Research (CICR),
Institute for Space-Earth Environmental Research (ISEE), Nagoya University,
Nagoya, Japan
Patricia H. Doherty (patricia.doherty_at_bc.edu)
SCOSTEP Scientific Secretary,
Boston College, Boston, MA, USA

Ramon Lopez (relopez_at_uta.edu)
PRESTO chair,
University of Texas at Arlington, TX, USA

Newsletter Secretary:

Mai Asakura (asakura_at_isee.nagoya-u.ac.jp)
Center for International Collaborative Research (CICR),
Institute for Space-Earth Environmental Research (ISEE), Nagoya University,
Nagoya, Japan

PRESTO co-chairs
and Pillar co-leaders:

Eugene Rozanov (co-chair), Jie Zhang (co-chair), Allison Jaynes (Pillar 1 co-leader), Emilia Kilpua (Pillar 1 co-leader), Spiros Patsourakos (Pillar 1 co-leader), Loren Chang (Pillar 2 co-leader),Duggirala Pallamraju (Pillar 2 co-leader), Nick Pedatella (Pillar 2 co-leader), Odele Coddington(Pillar 3 co-leader), Jie Jiang (Pillar 3 co-leader), and Stergios Misios (Pillar 3 co-leader)

SCOSTEP Bureau:

Kazuo Shiokawa (President), Daniel Marsh (Vice President), Nat Goplaswamy (Past President),
Patricia Doherty (Scientific Secretary), Aude Chambodut (WDS), Jorge Chau (URSI), KyungSuk Cho (IAU), Yoshizumi Miyoshi (COSPAR), Renata Lukianova (IAGA/IUGG), Peter
Pilewskie (IAMAS), Annika Seppälä (SCAR), and Prasad Subramanian (IUPAP)
website: www.bc.edu/scostep.

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SCOSTEP/PRESTO NewsletterVol. 30