SCOSTEP/PRESTONEWSLETTER
Vol. 28, July 2021

Inside this issue

Article 1:

Article 1:
1
Project “Role of the
Middle Atmosphere in
Climate” : Phase 2

Project “Role of the Middle Atmosphere in Climate” : Phase 2

Article 2:
3
Closure of the Onagawa
Magnetic Field Observatory of Tohoku University
Highlight onYoung Scientists 1:
Milla Kalliokoski/ Finland5

Highlight onYoung Scientists 2:
Yumi Bamba / Japan

7

Meeting Report 1:
8
44st Annual Seminar“Physics of the Auroral
Phenomena”,
Organized Online by PGI,
Apatity, Russia, 15-19
March 2021
Upcoming Meetings

9Franz – Josef Lübken1
1Director, Leibniz Institute for Atmospheric Physics (IAP) ,University of Rostock, Germany

Franz-Josef
LübkenThe atmosphere plays an important rolein climate change from global to regional scales. Especially in the middle
atmosphere, i. e., from the upper troposphere to the lower thermosphere (approx.
10 to 100 km), far-reaching changes due
to anthropogenic influences are alreadyobserved, and a further increase in the
coming decades is predicted. The importance of the middle atmosphere for the
climate is based on diverse interactions ofthese layers with the troposphere (approx.
0- 10 km) and can be roughly divided intoa) climate effects in the middle atmosphere, and b) influence of the middle atmosphere on the troposphere.

Changes in the composition of the middle atmosphere influence the radiation budget of the entire atmosphere andthus also the climate in the troposphere.
The middle atmosphere and troposphereare dynamically coupled with each otherin a variety of ways, especially by waves
on very different spatial and temporalscales. For a few years it is clear that not
only does the middle atmosphere react toanthropogenic activities, but that e.g.
stratospheric circulation changes can influence the regional climate.

In order to better understand the role ofthe middle atmosphere for climate andto be able to take it into account in future
projections, our understanding of these
coupling mechanisms must be improved.

Figure 1: Institutes involved in the second
phase of ROMIC (GEOMAR = Helmholtz Centre for Ocean Research,
IAP=Leibniz Institute of AtmosphericPhysics, MPMet = Max-Planck-Institutefor Meteorology, MPS = Max-PlanckInstitute for Solar System Research, FZ =Research Centre, KIT = Karlsruhe Institute of Technology, DLR/IPA = German
Aerospace Centre/Institute of Atmospheric Physics)

SCOSTEP/PRESTO Newsletter・Vol. 28

Article

The middle atmosphere is also a key region throughwhich changes in solar activity and large volcanic eruptions affect the climate. The importance of the middle
atmosphere for the troposphere becomes clear from thefact that weather services have meanwhile extended
their operational forecast models to the mesosphere(approx. 50-100 km) because this improves the predictions.

Highlight on Young Scientists

T

he German Federal Ministry for Education and Research (BMBF) has launched a program called ROMIC (Role Of the Middle atmosphere In Climate). The
first phase was successfully performed in the years 2014–2018. The second phase (ROMIC-2) started with someprojects in 2019, and in full extent in 2020. It is expected that ROMIC-2 will last until 2023.

T

he main research topics of ROMIC-2 are: i) Trends
in the middle atmosphere, ii) Forcing by solar radiation, greenhouse gases, and stratospheric aerosols, andiii) Coupling between the troposphere and the middle
atmosphere. These tasks are addressed in the following
8 projects where most of them are run by a speaker andseveral coinvestigators (CoI), usually from various institutes within Germany.

tät Frankfurt, Manfred Ern, FZ Julich, Oliver
Reitebuch, DLR-IPA, Oberpfaffenhofen

5.

Chemistry + trace gases
6.

SCI-HI (Surface Climate Impacts of Halogen Induced stratospheric ozone changes), Speaker:
Björn-Martin Sinnhuber, KIT, Karlsruhe, CoIs:
Andreas Engel, Universität Frankfurt, Jens-Uwe
Grooß, FZ Jülich, Klaus Pfeilsticker, Universität
Heidelberg

7.

TroStar (The transport of trace gases via the tropopause region in the Western Pacific observed by
FTIR spectrometry), Speaker: Mathias Palm, Universität Bremen

8.

SOCTOC (Effects of anthropogenic Stratospheric
Ozone Changes on climate sensitivity and Tropospheric Oxidation Capacity), Speaker: Hauke
Schmidt, MPMet, Hamburg, CoI: Roland Ruhnke,
KIT, Karlsruhe

Solar/climate variability + trends
1.

Meeting Report

SOLCHECK (Solar contribution to climate change
on decadal to centennial timescales), Speaker: Ulrike Langematz, FU Berlin, CoIs: Katja Matthes,
GEOMAR, Kiel, Holger Pohlmann, MPMet Hamburg, Miriam Sinnhuber, KIT, Karlsruhe.

2.

ISOVIC (Impact of SOlar, Volcanic and Internalvariability on Climate), Speaker: Ralf Koppmann,
Universität Wuppertal, CoIs: Claudia Timmreck,
MPMet Hamburg, Natalie Krivova, MPS, Göttingen.

3.

TIMA (Trends In the Middle Atmosphere), Speaker: Franz-Josef Lübken, IAP, Kühlungsborn.

Dynamics

Upcoming Meetings

4.

QUBICC (The Quasi-Biennial Oscillation in a
Changing Climate), Speaker: Marco Giorgetta,
MPMet, Hamburg, CoIs: Ulrich Achatz, Universi-

WASCLIM (Role of gravity WAves in the Southern hemispheric circulation and CLIMate), Speaker: Markus Rapp, DLR, Oberpfaffenhofen, CoIs:
Thomas Birner, LMU, München, Jorge Chau, IAP,
Kühlungsborn, Peter Preusse, FZ Jülich, Wolfgang
Woweide, KIT, KarlsruheAkickoff-meeting of the ROMIC-2 program took
place online on 26. February 2021. In total, morethan 100 scientists and students participated in thismeeting. ROMIC is part of BMBF’s high-tech strategy
for climate protection within the framework of researchfor sustainable development (FONA). The initiative
ROMIC is intended to help reduce existing uncertainties
in understanding climate and to allow for an important
step in the direction of improved predictability of climate change.

T

he scientists and institutes involved in ROMIC
thank the BMBF for introducing this funding opportunity. Although ROMIC concentrates on institutes
in Germany, international cooperation is highly recommended and results are presented (amongst others) in a
special session at the annual international EGU symposium in Vienna.

Announcement
Figure2: Some part of the participants in the ROMIC-2 online meeting held on 26. February 2021.

2

SCOSTEP/PRESTO Newsletter・Vol. 28

Article

Article 2:

Closure of the Onagawa Magnetic Field Observatoryof Tohoku UniversityT

he magnetic field observatory of Tohoku University at Onagawa Town in Miyagi Prefecture closed at
the end of March in 2021 with an illustrious history ofover 60 years. This article is an overview of the historyof the observatory during the past 60 years. Its various
scientific achievements are also highlighted.

T

Takahiro
Obara

Chile earthquake and tsunami struck Onagawa Town,
and the observation room and the magnetometer weredestroyed. So, the observatory was relocated to the current Kirigasaki location and it continued fully automated electronic measurement there. Research on the geomagnetic pulsation based on the magnetometer observations extensively progressed. The phenomenon “Pc” and“Pi” were named here. These names were certified by
the IAGA in 1971. They have become terms widelyused by researchers all over the world. Research on
magnetic pulsation has extensively progressed, especially in the studies of Pc-3 to Pc-5 and Pi-2 magnetic pulsations. More than one hundred scientific papers havebeen published up to now on these topics.

Meeting Report

he Onagawa Magnetic Field Observatory of Tohoku University was built at Kojyo-hama in 1947
with the assistance of Onagawa Town. Facilities areequipped with government building, a laboratory withabsolute observation room and a detector room. A stateof-the-art induction magnetometer and an electron tube
automatic equilibrium magnetometer were also installed. In 1957, the Onagawa observatory was assigned
as a magnetic pulsation pilot observatory. Since then,
Onagawa observatory has been internationally recognized as a leading magnetic observatory. Kojyo-hama
rapidly urbanized and precise measurements were injeopardy due to artificial disturbances. In 1960, theHighlight on Young Scientists

Takahiro Obara1
1PPARC, Tohoku UniversityT

he international research project STEP was started
in 1990, and Onagawa observatory played an important role as a key station of the observation network
along the geomagnetic longitude 210o. Joint research inJapan and overseas has been performed involving Nago-

Upcoming Meetings
Announcement

SCOSTEP/PRESTO Newsletter・Vol. 28

3Article
Highlight on Young Scientists
Meeting Reportya University, Kyushu University, Hokkaido University,
Tohoku Institute of Technology, and Stanford University.
In addition, the development of magnetometer mountedon "Akebono" satellite and an interplanetary probe"Sakigake" were performed by Prof. Fukunishi andProf. Saito, respectively.

Due to the reorganization of Tohoku University in
1999, Onagawa observatory was re-assigned to thePlanetary Plasma and Atmospheric Research Center(PPARC), and the new main building was opened in
2000. At that time, the Internet was connected, and thus

Upcoming Meetings
Announcement
4

SCOSTEP/PRESTO Newsletter・Vol. 28

fully automatic observation became possible and thisdata has been available on the website.

In the March of 2011, a massive earthquake caused themagnetometer to collapse, and it was ruined. The situation was getting worse because it hindered the maintenance of other observation equipment. Hence, unfortunately, it was closed at the end of March in 2021. Before
the closure of the observatory, Planetary Plasma and Atmospheric Research Center transferred the Kyushu University magnetometer to the site of Zao observatory at
the foot of Mt. Zao.

Article

Highlight on Young Scientists 1:

Impact of ICME Sheath Regions on Outer Radiation Belt Electrons

Turbulent sheath regions form in front of interplanetary coronal mass ejections (ICMEs). ICMEs are
key drivers of geomagnetic activity and variability in the
Earth’s outer radiation belt electron fluxes. The ICME
structures (shock, sheath and ejecta) have distinct impacts (Kilpua et al., 2017), and we focused on how
sheaths drive the radiation belt system in Kalliokoski etal. (2020).

S

Milla
Kalliokoskigies (10s to 100s keV) and deplete the high-energy (> 1
MeV) populations. The energy range where depletionoccurs narrows toward the heart of the outer belt, likely
caused by energy-dependent wave-particle interactions
dominating there, whereas losses at the magnetopause
with contributions from ULF-driven radial transport
dominate further out. We additionally found that sheaths
driving geomagnetic storms lead more often to both
energization and loss throughout the outer belt, but
nongeoeffective sheaths can also cause significant
changes in the outer belt electron fluxes.

To confirm the physical mechanisms determining theelectron dynamics during sheaths, we have continued this work with phase space density (PSD) analysis in
Kalliokoski et al. (2021). Fig. 2 compares the evolution

Meeting Reporttatistical study of 37 sheaths between 2012-2018
revealed elevated chorus and ultra-low frequency(ULF) wave activity during sheaths. In contrast to previous studies, we investigated the outer belt response immediately after the sheath to exclude variability causedby the ejecta. Fig. 1 shows the energy-dependence of the
response. Sheaths enhance electron fluxes at low ener-

Highlight on Young Scientists

Milla Kalliokoski
Department of Physics, University of Helsinki, Helsinki, Finland

Upcoming Meetings
Announcement

Figure 1: Percentage of sheaths causing enhancement, depletion or no significant changes in electron fluxes
throughout the outer belt at a wide range of energies observed by Van Allen Probes. The response is calculated as R = <post-sheath flux>/<pre-sheath flux> where <> denotes averaging over 6 hours.

SCOSTEP/PRESTO Newsletter・Vol. 28

5Articleof PSD radial profiles at ultrarelativistic energies during
two sheaths with opposite responses. The geoeffective
sheath (left) generated a growing peak in PSD, evidencing local acceleration by chorus. The nongeoeffective
sheath (right) led to effective magnetopause shadowing
via the combined process of magnetopause compression

and ULF-driven outward radial transport. Understanding the immediate outer belt response to different solar
wind drivers, regardless of their geoeffectiveness, is key
in forecasting the belt dynamics.

Highlight on Young Scientists
Figure 2: PSD radial profiles of nearly equatorially mirroring electrons at ultrarelativistic energies for (a) ageoeffective and (b) a nongeoeffective sheath. Each profile corresponds to an inbound or outbound pass ofthe two Van Allen Probes, color-coded by time as shown on the color bar.

Meeting Report

Acknowledgements
This work was supported by the Finnish Centre of Excellence in Research of Sustainable Space (Academy ofFinland grant 1312390). We thank the Van Allen Probes
team for making the electron flux data publicly available.
References

Upcoming Meetings

Kilpua, E. K. J., Koskinen, H. E. J., & Pulkkinen, T. I.
(2017). Coronal mass ejections and their sheath regionsin interplanetary space. Living Rev. Sol. Phys., 14(1), 5.
doi:10.1007/s41116-017-0009-6

Announcement
6

SCOSTEP/PRESTO Newsletter・Vol. 28

Kalliokoski, M. M. H., Kilpua, E. K. J., Osmane, A.,
Turner, D. L., Jaynes, A. N., Turc, L., George, H., Palmroth, M. (2020). Outer radiation belt and inner magnetospheric response to sheath regions of coronal mass ejections: a statistical analysis. A nn. Geophys., 38(3), 683701. doi:10.5194/angeo-38-683-2020

Kalliokoski, M. M. H., Kilpua, E. K. J., Osmane, A.,
Jaynes, A. N., Turner, D. L., George, H., Turc, L., Palmroth, M. (2021). Phase Space Density Analysis of Outer
Radiation Belt Electron Energization and Loss during
Geoeffective and Nongeoeffective Sheath Regions. ESSOAr. doi:10.1002/essoar.10507312.1 (preprint)

Article

Highlight on Young Scientists 2:

Exploring Small-Scale Magnetic Features That Trigger Solar Eruptions

Highlight on Young Scientists

Yumi Bamba1,2
1Institute for Advanced Research, Nagoya University
2Institute for Space-Earth Environmental Research, Nagoya University

Yumi
Bamba

olar eruptions, such as flares and coronal mass ejec- meters on the solar surface that is inferred to be caused
S
tions (CMEs), are sometimes disturb space environ- by a small magnetic disturbance was observed under thement around the Earth. However, it is not easy to fore- small flux rope. The big filament was disturbed just afterFI

the precursor brightening was observed, and it erupted
following an eruption of the small flux rope with a C2.4
flare (Figure 2d).
ur results suggest that the big filament eruption withseveral diameters of the Earth was triggered by thetiny (only a few hundred kilometers on the solar surface)magnetic disturbance. Further, the magnetic disturbancecan be represented by the small and transient precursor
brightening. Therefore, analysis of magnetic field change(spatial and temporal) and corresponding precursor
brightening is effective to identify a “trigger” of solar
eruptions.

O

Meeting Reportcast when solar eruptions occur because eruption onset ishighly sensitive to very small magnetic disturbance thesolar surface.
or instance, the largest magnetic storm in solar cycle
24, so-called the St Patrick's day storm, is originatedin a tiny magnetic disturbance that triggered a huge filament eruption on 15 March 2015 in solar active region(AR) NOAA 12297 (Bamba et al. 2019). Magnetic fieldstructure surrounding the AR was complicated: several
filaments including big filament that erupted (Figure 1a)were rooted in the AR. Especially, closed magnetic fields
that sustained the erupting big filament rooted into northof a satellite sunspot (Figure 1b). Additionally, there islocally but highly twisted magnetic structure, i.e., small
magnetic flux rope existed at the northern end of the satellite sunspot, and it was represented by a small filament(Figures 1a, 1b).
t is noteworthy that a tiny precursor brightening(Figure 1c) with a spatial scale of a few hundred kilo-

Reference
Bamba Y., Inoue S., and Hayashi K., 2019, The Astrophysical Journal, 874:73 (11pp), doi: 10.3847/15384357/ab06ff

Upcoming Meetings
Announcement

Figure 1: Global and local structures of the AR 12297. (a) The big filament that erupted and the small filament. (b) Magnetic field structures in/around the AR. There was the small magnetic flux rope that corresponding to the small filament in the north of the satellite sunspot. (c, d) The precursor brightening (in panelc) and the C2.4 flare ribbons (in panel d) in the chromosphere. The tiny precursor brightening that represents a small magnetic disturbance was observed approximately an hour before the C2.4 flare onset.

SCOSTEP/PRESTO Newsletter・Vol. 28

7Article
Highlight on Young Scientists

Figure 2: Temporal variation of the erupting big filament observed by SDO/AIA193Å. (a) The erupting big
filament is marked by the shite arrow. The line cut is over plotted by the white line. (b) Time-slice image ofthe erupting big filament, for the period of 20:00 UT on March 14 to 03:00 UT on 2015 March 15. The C2.4
and C9.1 flaring time is indicated by the vertical blue and green lines, respectively. The duration of the small
precursor brightening is indicated as between the vertical white dashed lines.

Meeting Report 1:

Meeting Report

44st Annual Seminar “Physics of the Auroral Phenomena”, Organized Online by PGI, Apatity, Russia, 15 - 19 March 2021

Andrei Demekhov1
1Polar Geophysical Institute, Apatity, Russia

Upcoming MeetingsThe 44st Annual Seminar “Physics of the auroral phenomena” has been held online during 15-19 March
2021. The organizer of the Seminar is the Polar Geophysical Institute (PGI) in Apatity (Murmansk region,
Russia).

M

Announcement

ore than 90 representatives from 20 research institutes and universities distributed across Russia(from Kaliningrad to Yakutsk) took part in the Seminar.
Of those, more than 25 people are young scientists from
Moscow, St. Petersburg, Kaliningrad, Irkutsk, Apatity,
and Murmansk. Among the participants there wereabout 20 representatives of foreign research institutes, ofwhom 11 persons (from Argentina, Bulgaria, India,
USA, Czech Republic, and Japan) presented their reports. Such a broad participation of foreign scientists inthis mostly Russian event has become possible becauseof its online format and due to its announcing via
SCOSTEP mailing list and personal communications.
oral and 58 poster presentations were delivered.
6talks,7Posters
were presented as short (5 min) elevation
accessed online, and discussed at evening sessions
in Spatialchat.

T
8

he Seminar is devoted to the discussion of the latest
results obtained by Russian and foreign scientists on

SCOSTEP/PRESTO Newsletter・Vol. 28

Andrei
Demekhovthe physical processes in the polar cap, auroral, and subauroral regions, in the solar wind, magnetosphere, ionosphere, and atmosphere. The Seminar subjects cover all
aspects of the solar-terrestrial relations: 1) Storms andsubstorms; 2) Fields, currents, particles in the magnetosphere; 3) Waves, wave-particle interaction; 4) The sun,the solar wind, cosmic rays; 5) The ionosphere and theupper atmosphere; 6) Lower atmosphere, ozone; 7) Heliobiosphere.

T

he SCOSTEP/PRESTO program was a co-sponsorof the Seminar and partially supported the preparation of our online meeting, such as upgrading zoom license, purchasing Spatialchat license, developing web
pages for poster viewing and accessing the presentations,archiving the presentations, reserving DOI for the seminar proceedings, etc. The final Seminar program is available at http://pgi.ru/apsem2021/?id=prog, and the bookof abstracts can be found at http://pgia.ru/seminar/
abstracts_book2021.pdf. The Seminar will be followedby publication of the proceedings, which will be available both online at http://pgia.ru/seminar/archive/ and in
print. The electronic version of the seminar proceedings
is published by the Russian Science Electronic Library(https://elibrary.ru/title_about.asp?id=57098).

Date

LocationContact Information

The first summer school on space research,technology and application in Bulgaria

Jul. 5-11, 2021

National Observahttps://bulgarianspace.online/
tory Rozhen, South
space-schoolbg-2021/
of Bulgaria

ISWI/SCOSTEP Iberian Space Science
Summer School

Jul. 26-30, 2021

Onlinehttps://www.i4s-iberian-spacescience-summer-school.com/

Suntec, Singapore

IAU 2021 General AssemblyAug. 16-27, 2021

Busan, Korea

http://www.iauga2021.org/

IAGA 2021

Aug. 22-27, 2021

Hyderabad, India

http://www.iaga-iaspeiindia2021.in/

URSI GASS 2021

Aug. 28- Sep.4,
2021

Rome, Italy

https://www.ursi2021.org/

The 30th IUPAP General Assembly

Oct. 20-22, 2021

Beijing, China

http://iupap-ga2020.cpsnet.org.cn/

AGU Fall Meeting 2021

Dec. 13-17, 2021

New Orleans, LA,
USA

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

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

Feb. 21-25, 2022

Alibag, India

https://www.stp15.in/

EGU General Assembly 2022

Apr. 3-8, 2022

Vienna, Austria

https://www.egu22.eu/

COSPAR 2022

Jul. 16-24, 2022

Athens, Greece

http://ww.cosparathens2022.org/

Aug. 14-19, 2022

Melbourne,
Australia

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

AOGS 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

In July, 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

Announcement

SUMMER SPACE WEATHER SCHOOL - Physics
In October, 2022
and use of tools

Upcoming Meetings

Aug. 1-6, 2021

Meeting Report

AOGS 2021

https://www.asiaoceania.org/
aogs2021/public.asp?
page=home.html

Highlight on Young Scientists

Conference

ArticleUpcoming meetings related to SCOSTEP

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

SCOSTEP/PRESTO Newsletter・Vol. 28

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:

Miho Sugiyama (sugiyama.miho_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: https://scostep.org

10

SCOSTEP/PRESTO Newsletter・Vol. 28