SCOSTEP/PRESTONEWSLETTER
Vol. 36, July 2023

Inside this issue
Article 1:
New Findings on Equatorial Plasma Bubbles(EPBs) Morphology by
GOLD Mission

1

Article 2:
The Advanced SpaceBased Solar Observatory(ASO-S)—contributing
data to PRESTO

3

Highlight onYoung Scientists 1:
Tinatin Baratashvili /Belgium

4

Highlight onYoung Scientists 2:
Evangelia Samara
/ USA

5

7
Meeting Report 1:
ICTP-SCOSTEP-ISWI
School and Workshop on
the Predictability of the
Solar-Terrestrial Coupling – PRESTO
Upcoming Meetings

8

Announcement 1:
SCOSTEP 2023 Distinguished Service Award

9

Announcement 2:
International Science
Council (ISC) Members’
Forum in Paris, 10-12
May 2023

10

Announcement 3:
SCOSTEP Bureau meeting on 11 July 2023

10

Announcement 4:
SCOSTEP General Council Meeting on 14 July
2023

11

Article 1:

New Findings on Equatorial Plasma Bubbles (EPBs) Morphology by GOLD Mission

Deepak Kumar Karan1
1University of Colorado, Boulder, CO, USAN

ASA’s Global-scale Observationsof the Limb and Disk (GOLD) mission observes the Earth’s upper atmosphere from the geostationary orbit at
47.5°W longitude. GOLD makes disk
and limb observations, and occultations
at FUV emission wavelength (~132–162nm). It observes the American, Atlantic,
and West African longitudinal regions.
The instrument and its observations are
discussed in Eastes et al., (2020) and
McClintock et al., (2020). In thenighttime mode, GOLD takes OI 135.6
nm emission partial disk scans from ~10°

Deepak Kumar
Karan

E to ~80°W longitudes multiple times
between 19 to 22 Local Times (LTs).
These images provide a unique opportunity to unambiguously observe the spatial-temporal evolution of various
nighttime
ionospheric-thermosphericfeatures, such as the Equatorial Ionization Anomaly (EIA) and Equatorial Plasma Bubbles (EPBs). GOLD’s observations on these features have added new
insights to our previous understanding
and have opened up new directions andchallenges for our research community.

Figure 1. The only two cases when GOLD observed occurrences of consecutive Cshape, straight, and reversed C-shape EPBs within (A) 12o and (B) 6o longitudes.

SCOSTEP/PRESTO NewsletterVol. 36

12 October 2020

ArticleHighlight on Young Scientists
Meeting Report
Upcoming Meetings

Magnetic Latitude Zone

B1

B2

B3

B4

B5

N-EIA crest

65 ± 262 ± 457 ± 9115 ± 20123 ± 16

Equator48 ± 662 ± 268 ± 4125 ± 788 ± 14

S-EIA crest

62 ± 361 ± 552 ± 5108 ± 3104 ± 14

Table 1. EPBs’ zonal drift velocities (m/s) at the magnetic equator, N and S EIA crest latitudes on 12 October 2020
and 26 December 2021. Positive drift velocities are eastward.

One of these findings is the occurrence of differently
shaped EPBs within a small (~6o) longitude (Karanet al., 2023). On 12 October 2020, GOLD observed
three consecutive EPBs; a C-shape, a straight, and areversed C-shape EPBs, within ~12o longitudes at magnetic equatorial latitudes (Figure 1A). In another caseon 26 December 2021, a reversed C-shape and C-shape
EPB were observed sidewise within ~6o longitudes(Figure 1B). While there are numerous images of thedifferent shapes EPBs, these two examples of consecutive EPBs with opposite shapes within a small longitude
range are unusual. We calculated EPBs’ zonal drift velocities as explained in Karan et al., (2020). The drift
velocities are eastward at the magnetic equator and EIA
crests but with different magnitudes (Table 1). The latitudinal variations of the drift velocities agree with the
EPBs’ shape. This could be due to the latitudinal/
altitudinal variations of the zonal wind speeds that drive
their motions. Also, the inter-bubble separations corroborated these findings. The important finding here is theoccurrence of different EPBs’ shapes in such small(~6o) longitude ranges which indicate small-scale longitudinal differences in the E-region density, electricfield, neutral wind variations, or a combination of them.
Using optical dayglow emission, Karan and Pallamraju(2017), for the first time, reported the existence of small
spatial scale variations (~3o longitude) in the daytime
equatorial electric fields. The present observation could
be due to such variations of electric fields but during
after sunset hours. These rare and unique observations
are crucial for a better understanding of plasma irregularities and provide a challenge for numerical simulations to advance our understanding of the I-T system.

Another finding is the simultaneous observations ofgeomagnetic storm effects on the EIA morphology
and EPBs occurrence rate from the geostationary orbit(Karan et al., 2023). During the main phase of a storm
on 27 September 2020, the EIA crests were shifted 8°–
10° poleward compared to the quiet time monthly meanacross ~65°–35°W and an increase in EPB occurrence
rate is observed. Concurrent increase of hmF2 fromdigisonde observation confirms the strengthening of theplasma fountain effect during postsunset hours.

Announcement2

26 December 2021

SCOSTEP/PRESTO NewsletterVol. 36

References:
1) Eastes, R. W., McClintock, W. E., Burns, A. G.,
Anderson, D. N., Andersson, L., Aryal, S., et al.
(2020). Initial observations by the GOLD mission. J.
Geophys. Res. Space Physics, 125, e2020JA027823,
doi:10.1029/2020JA027823

2) McClintock, W. E., Eastes, R. W., Beland, S., Bryant, K. B., Burns, A. G., Correira, J., et al (2020).
Global‐scale Measurements of the Limb and Disk
(GOLD) Mission Implementation: 2. Observations,
Data Pipeline and Level 1 Data Products. Journal ofGeophysical Research: Space Physics, 125,e2020JA027809.
https://
doi.org/10.1029/2020JA027809.
3) Karan, D. K., and D. Pallamraju, (2017). Small-scale
longitudinal variations in the daytime equatorial
thermospheric wave dynamics as inferred from oxygen dayglow emissions. J. Geophys. Res. Space
Physics,
122,6528-6542,
doi:10.1002/2017JA023891

4) Karan, D. K., Daniell, R. E., England, S. L., Martinis, C. R., Eastes, R. W., Burns, A. G., &McClintock, W. E. (2020). First zonal drift velocity
measurement of equatorial plasma bubbles (EPBs)
from a geostationary orbit using GOLD data. J. Geophys. Res. Space Physics, 125, e2020JA028173,
doi:10.1029/2020JA028173
5) Karan, D. K., R. W. Eastes, C. Martinis, et al.
(2023), Unique Combinations of Differently Shaped
Equatorial Plasma Bubbles Occurring Within a
Small Longitude Range. ESS Open Archive. DOI:
10.22541/essoar.168500365.58259329/v1
6) Karan, D. K., Eastes, R. W., Daniell, R. E., Martinis,
C. R., & McClintock, W. E. (2023). GOLD mission's observation about the geomagnetic storm effects on the nighttime equatorial ionization anomaly(EIA) and equatorial plasma bubbles (EPB) during asolar minimum equinox. Space Weather, 21,e2022SW003321.
https://
doi.org/10.1029/2022SW003321

Article

Article 2:

The Advanced Space-Based Solar Observatory (ASO-S)—
contributing data to PRESTO

T

A

T

he scientific objectives of ASO-S can be briefly
expressed as 1M2B, where M stands for solar magnetic field, and 2B stand for two bursts, solar flares andcoronal mass ejections (CME), that is, to observe simultaneously the solar magnetic field, solar flares, andCME, so as to study their formation, evolution, interac-tion and possible causal relationship among them. The
innovation points of ASO-S include: (1) 1M2B scientific goals and thereby three payload deployments; (2)on a single near-Earth platform to perform a joint observation of the full disc vector magnetic field, solar nonthermal imaging, and CME’s formation and early propagation; (3) to observe in Lyman-alpha waveband fromthe full disc of the Sun seamlessly to 2.5 solar radius.

In order to fulfil the scientific goals, three payloads are
deployed, which are the Full-disc vector MagnetoGraph (FMG) for observing the full Sun vector magnetic field, solar Hard X-ray Imager (HXI) for observing
the non-thermal morphology of solar flares and imaging
spectra, and Lyman-alpha Solar Telescope (LST) for
observing both the formation and early propagation of
CME, respectively. Figure 1 shows the layout of ASOS.

On October 9, 2022, ASO-S was sent by a Long
March 2D rocket into a Sun-synchronous orbit
with an altitude of 720 km, inclination angle of 98.27o,ascending node 6:00 am, eccentricity of zero, and period
of about 99 minutes (Figure 2). After the commissioning
phase of 6 months, most of the data together with thedata software is now opened to the community via thehome page at http://aso-s.pmo.ac.cn/en_index.jsp. The
first light can be found at Gan et al. (2023).

Upcoming Meetingss a matter of fact, 2011 is the first year of an era forthe scientific satellite in China, when a new program named Strategic Priority Research Program on
Space Science, led by CAS, was formed. Being the second batch of mission candidates, ASO-S was grantedwith the conception study in 2011, and then in 2014
with the background study (feasibility). In the end of
2017, ASO-S was finally approved by CAS. Afterwards,
undergoing almost 5 years engineering phases, the ASO-S was successfully launched on October 9, 2022, being
the first comprehensive solar mission in China (Gan etal., 2022).

Weiqun Gan

Meeting Report

he earliest attempt for solar observation from spacein China could traceback to the 70’s last century,
when the “Astron-1” mission was proposed and performed. Then in the early 90’s last century, a package ofthree instruments aiming at observing the high energy
radiation from the the Sun, was implemented and sent
into the orbit on January 10, 2001, on board the Shenzhou-2 spacecraft. At the same period of the time orlater, there were also some other proposals (Gan et al.
2019), like the Space Solar Telescope, SMESE (SMall
Explorer for Solar Eruptions, a joint Chinese-French
mission), Kuafu mission, and so on. All these proposals
did not arrive at the engineering phases at the time moment of around 2010, when ASO-S was proposed.

Highlight on Young Scientists

Weiqun Gan1
1Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing, China

Announcement

Figure 2. ASO-S was being launched on 9 October
2022.

T
Figure 1. ASO-S before the launch.

he lifetime of ASO-S is designed to be no less than
4 years, so that it covers well the peak years of the25th cycle of solar activity. In order to encourage tomake use of the data, ASO-S team recently issued theGuest Investigator Program, in which 8 to 12 guest investigators could be invited to visit ASO-S data centerfor 2-3 months, to perform independent or joint researches based on the ASO-S data.

SCOSTEP/PRESTO NewsletterVol. 363

References

ArticleGan, W. Q., Zhu, C., Deng, Y. Y., Li, H., Su, Y., Zhang,
H. Y., et al. (2019), Advanced Space-based Solar Observatory (ASO-S): an overview. Research in Astronomy
andAstrophysics,
19,
156.
https://
doi.org/10.1088/1674-4527/19/11/156

Highlight on Young Scientists
Meeting Report
Upcoming Meetings
Announcement
4Gan, W. Q., Feng, L., & Su, Y. (2022), A Chinese solar
observatory in space, Nature Astronomy, 6, 165. https://doi.org/10.1038/s41550-021-01593-9
Gan, W. Q., Zhu, C., Deng, Y. Y., Zhang, Z., Chen, B.,
Huang, Y., et al. (2023), The Advanced Space-Based
Solar Observatory (ASO-S), Solar Physics, 298, 68.
https://doi.org/10.1007/s11207-023-02166-x

Highlight on Young Scientists 1:

Icarus: 3D Heliospheric Modelling with Radial Grid Stretchingand Adaptive Mesh Refinement

Tinatin Baratashvili1 and Stefaan Poedts1, 2
1Centre for Mathematical Plasma Astrophysics, Leuven, Belgium
2Institute of Physics, University of Maria Curie-Skłodowska, Lublin, PolandCoronal mass ejections, when directed towards
Earth, can cause significant damage to our home(a) CME tracing

Tinatin
Baratashvili

StefaanPoedtsplanet. In order to mitigate the damage coming fromsuch events, forecasting tools are necessary.

(b) Shock tracing(c) Combined

Figure 1. AMR criteria available in Icarus. (a) CME tracing criterion is implemented for controlling the refinement in the domain. (b) The shock areas are refined in the domain and in (c) both the CME interior and shock arerefined by combining (a) and (b) criteria.

A

new 3D heliospheric model, Icarus (Verbeke et al.,2022) was recently developed with the access toadvanced techniques, such as grid stretching and adaptive mesh refinement (AMR). Icarus covers the heliosphere from 0.1 AU to 2 AU and provides time varying
conditions of various plasma quantities at multiple

points in the domain and 3D modelled data of the heliosphere with solar wind and propagating coronal massejections (CMEs) in it. Currently, a simple hydrodynamics CME model and a more advanced, magnetized
CME model are available to inject in the heliospherefrom the inner boundary in Icarus.

Shockrefinement

AMR 3;
Grid Stretching

AMR 4;
Grid Stretching

AMR 5;
Grid Stretching

0h 11m0h 27m2h 39mMiddle Resolusion; AMR 2;
Equidistant
Grid stretching

Wall-click Time 6h 16m

0h 8m

Table 1. The table shows the wall-clock times simulations take when performed on 1 node with 36 CPUs on the
Genius cluster of Vlaams Supercomputing Centre. The shock refinement criterion is used in the simulations with
AMR and grid stretching. Middle equidistant resolution simulation is usually an operational setting for heliospheric forecasting, therefore it is taken as a reference.

SCOSTEP/PRESTO NewsletterVol. 36

Table 1 displays the times required for different
AMR level simulations and a middle equidistantsimulation, for a reference. The speed-up obtained withusing advanced techniques, depending on the AMR level and criterion, can vary from 3 to 35. Thus, heliospheric modelling is optimized in Icarus and bearing this inmind, we are developing more realistic flux-rope models and a time-accurate solar wind model.
References:

Highlight on Young Scientists

dvanced techniques, such as grid stretching and
AMR, guarantee the efficiency of the simulations.
Gradual radial grid stretching maintains the fixed aspectratio in the domain, while AMR achieves high resolution in the domain only where necessary. AMR can becontrolled by an implemented criterion, thus it can besuited for various purposes. Fig 1 gives an overview ofdefault AMR criteria in Icarus, which is presented in
Baratashvili et al., 2022. Fig 1(a) shows the refined domain according to the CME interior tracing function, fig
1(b) shows the refinement of the shock areas in the domain and fig 1(c) combines the first two criteria.

ArticleA

Baratashvili, T., Verbeke, C., Wijsen, N. and Poedts, S.,
2022, A&A, 667, A133.
Verbeke, C., Baratashvili, T., & Poedts, S. 2022, A&A

Highlight on Young Scientists 2:

Geometrical complexity of coronal holes: how does it affectthe fast component of the solar wind observed at Earth?

Meeting Report

Evangelia Samara1
1NASA/Goddard Space Flight Center, Greenbelt, MD, USA

Evangelia
SamaraI

Announcement

Figure 1. Three different fits are applied to the same
CH sample. A medium Pearson’s correlation coefficient (c = 0.50) indicates the non-ideal linear fitting of
the blue line to the entire dataset. A higher Pearson’s
correlation coefficient (c = 0.70) results from the linear
fitting of the red line to small CHs, up to CH size of 6.4
x 1010 km2 (grey dashed line). A power-exponentialfunction (light-green) is more appropriate to describe
the dataset as it has the meaning that the HSS peakvelocity cannot increase without restrictions.

Upcoming Meetings

t is long known that the peak velocity of the highspeed solar wind streams (HSSs) recorded at Earthcorrelates with the area of their source region on theSun, i.e., the coronal holes (CHs). Many authors havesupported the linear association between the two characteristics (see e.g., Nolte et al. 1976; Vršnak et al. 2007;
Abramenko et al. 2009; Karachik & Pevtsov 2011; Rotter et al. 2012; Hofmeister et al. 2018; Heinemann et al.
2020). However, this is not always the case. A linear
association is more consistent for small CH sizes, but if
we go towards bigger CHs we meet a threshold beyond
which, no matter the CH growth, there is no further increase in the HSS peak velocity observed at Earth. This

Figure 2. HSS peak velocity recorded at Earth as afunction of the CH area on the Sun for different FD
ranges, going from the least complex (top panel) to themost complex (bottom panel) CHs.

SCOSTEP/PRESTO NewsletterVol. 365

Article
Highlight on Young Scientists

is noticeable in Figure 1, where a threshold in speeds isrecorded around 630 km/s. A blue line is fitted to thedataset of 45 non-polar CHs (blue points) and a red line
only to small CH sizes (up to 6.4 x 1010 km2). None ofthem is adequate to describe the entire sample, therefore
applying a power-exponential function seems more appropriate. This is because, among all fitting curves, thepower-exponential one has the meaning that the HSS
peak velocity cannot increase without restrictions. But
what are those restrictions?

3) Georgoulis, M. K. (2012). Are solar active regionswith major flares more fractal, multifractal, or turbulent than others?. Solar Physics, 276, 161-181.

T5) Hofmeister, S. J., Veronig, A., Temmer, M., Vennerstrom, S., Heber, B., & Vršnak, B. (2018). The dependence of the peak velocity of high‐speed solar
wind streams as measured in the ecliptic by ACE
and the STEREO satellites on the area and co‐latitude of their solar source coronal holes. Journalof Geophysical Research: Space Physics, 123(3),1738-1753.

o answer this question, the geometrical complexityof the CHs is quantified by calculating the fractal
dimension (FD) of their contours (Georgoulis 2005,2012). As the contours become more ragged and irregular, the complexity of the CH grows, and as a result, its
FD. In our sample, the FD ranges between 1.1 – 1.4.
Therefore, we divide the dataset in three subgroups
based on their FD, as seen in Figure 2. We notice thatthe linear association in the HSS peak velocity – CH
area plot decreases as the FD increases, namely, the linear association becomes poorer when we go from theleast towards the most complex structures.

O

Meeting Reportur findings show that as a CH grows, its complexity grows with it preventing the preservation of ahomogeneous, uniform shape. This, in turn, prevents thegeneration of faster solar wind, which is supposed tooriginate from the most compact, homogeneous part of
the CH. Therefore, the threshold seen in Figure 1 (andin similar other figures), can be explained. The robustness of these results has been verified by the pair bootstrapping technique. For more details, see Samara et al.,2022 (Astronomy & Astrophysics).
References:1) Abramenko, V., Yurchyshyn, V., & Watanabe, H.
(2009). Parameters of the magnetic flux inside coronal holes. Solar Physics, 260, 43-57.

Upcoming Meetings

2) Georgoulis, M. K. (2005). Turbulence in the solar
atmosphere: Manifestations and diagnostics via solar
image processing. Solar Physics, 228, 5-27.

Announcement
6

SCOSTEP/PRESTO NewsletterVol. 36

4) Heinemann, S. G., Jerčić, V., Temmer, M., Hofmeister, S. J., Dumbović, M., Vennerstrom, S., ... & Veronig, A. M. (2020). A statistical study of the longterm evolution of coronal hole properties as observed by SDO. Astronomy & Astrophysics, 638,
A68.

6) Karachik, N. V., & Pevtsov, A. A. (2011). Solarwind and coronal bright points inside coronalholes. The Astrophysical Journal, 735(1), 47.
7) Nolte, J. T., Krieger, A. S., Timothy, A. F., Gold, R.
E., Roelof, E. C., Vaiana, G., ... & McIntosh, P. S.
(1976). Coronal holes as sources of solar wind. Solar
Physics, 46, 303-322.
8) Rotter, T., Veronig, A. M., Temmer, M., & Vršnak,B. (2012). Relation between coronal hole areas on
the Sun and the solar wind parameters at 1 AU. Solarphysics, 281, 793-813.
9) Samara, E., Magdalenić, J., Rodriguez, L., Heinemann, S. G., Georgoulis, M. K., Hofmeister, S. J., &Poedts, S. (2022). Influence of coronal hole morphology on the solar wind speed at
Earth. Astronomy & Astrophysics, 662, A68.
10)Vršnak, B., Temmer, M., & Veronig, A. M. (2007).
Coronal holes and solar wind high-speed streams: I.
Forecasting the solar wind parameters. Solar Physics, 240(2), 315-330.

Article

Meeting Report 1:

ICTP-SCOSTEP-ISWI School and Workshop on the Predictability of the Solar-Terrestrial Coupling – PRESTO

Sharafat
Gadimova

he ICTP-SCOSTEP-ISWI School and Workshop
were held during May 29 - June 2, 2023 at the Abdus Salam ICTP, Trieste, Italy. This was the first fullface-to-face/in-person meeting since the PRESTO program was launched in 2020. On the first day, the school
was composed of six 1-hour lectures related to the three
PRESTO Pillars. The 4-day workshop that followed the
School had seven sessions: 1) Observations and modelling of solar eruptions, solar wind and SEPs from the
Sun through the interplanetary space, 2) Prediction ofsolar transients, streams/SIRs and SEPs from the Sun togeospace, 3) Effect of space weather on the Earth's ionosphere, thermosphere, and magnetosphere system, 4)

Keith M.
GrovesRamon Lopez

Bruno Nava

Kazuo
Shiokawa

Influence of the lower atmosphere on the mesosphere,
thermosphere, and ionosphere, 5) Solar forcing specification and impacts on the atmosphere and climate, 6)
Precipitating energetic particles and their effects on atmosphere, and 7) Predictability of the solar cycle.
Eighty-three participants from 39 countries and regions
attended the school and workshop. The school andworkshop were sponsored by the SCOSTEP/PRESTO
program, ICTP, ISWI, ICG, Boston College, Japan Society for the Promotion of Science (JSPS) (core-to-coreprogram for Asia-Africa platform), and ISEE, Nagoya
University.

Meeting ReportT

Natchimuthuk
Gopalswamy

Highlight on Young Scientists

Sharafat Gadimova1, Natchimuthuk Gopalswamy2, Keith M. Groves3, Ramon Lopez4, Bruno Nava5 andKazuo Shiokawa6
1International Committee on Global Navigation Satellite Systems (ICG) / United Nations Office for Outer
Space Affairs (UNOOSA), Vienna, Austria
2International Space Weather Initiative (ISWI) / NASA GSFC, Greenbelt, MD, USA
3SCOSTEP / Boston College, Boston, MA, USA
4PRESTO / University of Texas at Arlington, Arlington, TX, USA
5The Abdus Salam International Centre for Theoretical Physics (ICTP), Trieste, Italy
6SCOSTEP / Institute for Space-Earth Environmental Research (ISEE), Nagoya University, Nagoya, Japan

Upcoming Meetings
Announcement

Figure 1. School participants (left) and workshop participants (right) .

SCOSTEP/PRESTO NewsletterVol. 367

Article

Upcoming meetings related to SCOSTEPHighlight on Young Scientists

Conference

Date

LocationContact Information

The AGATA Kick-off meeting

Jul.12, 2023

Germany

www.scar.org/science/agata/home

XXXVth URSI General Assembly and Scientific Symposium

Aug. 19-26, 2023

Sapporo, Japan

https://www.ursi-gass2023.jp/

6th African Geophysical Society (AGS) International Conference on “Advancing Science Oct. 2-4, 2023
& Technology in Developing Nations

Lusaka, Zambia

https://afgps.org/conference

International Colloquium on Equatorial and
Low Latitude Ionosphere (ICELLI 2023)

Sep. 4-8, 2023

Ilorin, Nigeria

https://arcsstee.org.ng/
colloq2023/

The 2023 IMCP Space Weather School

Sep. 14-23, 2023

Beijing, China

http://imcp.ac.cn/en/
coop/2023IMCP/anno/xs1
https://iswi-secretariat.org/iswispace-weather-school-zambia2023/

Meeting Report

The International Space Weather Initiative
SchoolSep. 26-30, 2023

Lusaka, Zambia

Space Weather and Upper Atmospheric
Data analysis Training Workshop for East
African Community

Oct. 2-6, 2023

Arua, Uganda

Upcoming Meetings

The 2023 Sun-Climate Symposium

Oct. 16-20, 2023

Flagstaff, AZ, USA

https://lasp.colorado.edu/
meetings/2023-sun-climatesymposium/

The European Space Weather Week
(ESWW)

Nov. 20-24, 2023

Toulouse, France

http://esww2023.irap.omp.eu/

AGU Fall Meeting 2023

Dec. 11-15, 2023

San Francisco, CA,USA

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

IAU Symposium 388: Solar and Stellar CoroMay 5-10, 2024
nal Mass ejections

Krakow, Poland

https://
iausymposium.zyrosite.com/

45th COSPAR Scientific Assembly

Jul. 13-21, 2024

Busan, South Korea

https://www.cospar2024.org/

XXXII IAU General AssemblyAug. 5-16, 2024

Cape Town, South
Africahttps://www.iau.org/science/meetings/future/symposia/

11th SCAR Open Science Conference

Aug. 19-23, 2024

Pucon, Chile

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

Announcement
8

SCOSTEP/PRESTO NewsletterVol. 36

Announcement 1:

ArticleSCOSTEP 2023 Distinguished Service AwardSCOSTEP is pleased to announce that theHighlight on Young Scientists

2023 Distinguished Service Award is given to

Dr. Marianna G. Shepherd
York University, Toronto, Canada

Marianna G.
Shepherd

Citation: For unique and meritorious service to SCOSTEP activities and interests at an international level, particularly for her work in the position of the Scientific Secretary of SCOSTEP.

D

D

r. Shepherd assisted with the management andevents for the CAWSES II and VarSITI scientificprograms. She organized, prepared and managed
SCOSTEP Newsletters from 2013 to 2019 and preparedbrochures on SCOSTEP and VarSITI. She also organized and managed elections for SCOSTEP executives
in 2011, 2015 and 2019. Dr. Shepherd designed andmanaged the first website for SCOSTEP. She also organized a digital archive of all SCOSTEP documents andactivities.

T

his award recognizes Dr. Shepherd’s many uniqueand meritorious services to SCOSTEP activities,
particularly her work as Scientific Secretary of
SCOSTEP, which contributed much to successful running of SCOSTEP and its projects and to a better visibility of SCOSTEP in the international scientific community.

Upcoming Meetings

r. Shepherd represented SCOSTEP at many events
including two AGU Town Hall meetings. She also
gave presentations on SCOSTEP and its relevant scientific programs at the Scientific and Technical Subcommittee (STSC) meetings at the United Nations Committee on the Peaceful Uses of Outer Space (UNCOPUOS)
held in Vienna in 2012, 2014 and 2015. Dr. Shepherd
was instrumental in SCOSTEP’s successful application
for Permanent Observer status at the COPUOUS in
2012 – giving SCOSTEP a seat at future STSCCOPUOS meetings. These activities contributed to thesuccess and visibility of SCOSTEP and its scientificprograms.

D

Meeting Reportr. Marianna G. Shepherd served SCOSTEP as Scientific Secretary from 2010 to 2019. In this role,
Dr. Shepherd organized and oversaw the day-to-day
financial and administrative operations of SCOSTEP. In
addition, Dr. Shepherd organized and managed the annual SCOSTEP Visiting Scholars program; the Capacity
Building activities; and assisted in the organization of
the 13th Quadrennial Solar-Terrestrial Physics Symposium, Xi’an, China in October 2014. She also served as
the main local organizer of the 14th Quadrennial SolarTerrestrial Physics Symposium in Toronto, Canada inJuly 2018.

Announcement

SCOSTEP/PRESTO NewsletterVol. 369

ArticleAnnouncement 2:

International Science Council (ISC) Members’ Forum in Paris,
10-12 May 2023

Highlight on Young Scientists

Kazuo Shiokawa (SCOSTEP President)1
1Institutefor Space-Earth Environmental
Nagoya, Japan

Research(ISEE),

NagoyaUniversity,

Kazuo
Shiokawa

S

Meeting Report

COSTEP is one of the Affiliated Bodies (a thematicorganization) of the International Science Council(ISC). The mid-term meeting of ISC members“Capitalizing on Synergies in Science” was held at Novotel Paris Centre Tour Eiffel in Paris, France, on 10-12
May 2023, and I joined this meeting as the SCOSTEPPresident. Details of the meeting is available at https://council.science/events/2023-members/. About threehundred delegates representing the global scientificcommunity from 80 countries joined this meeting. At
the beginning of the meeting, the ISC President, Dr.
Peter Gluckman talked about the present and future of
the ISC. ISC is newly collaborating with the United Nations and newly launched the ISC’s Centre for Science
Futures. On the morning of the day 3 (May 10) a session
for the Affiliated Bodies of ISC was held where all the
Affiliated Bodies, including SCOSTEP, reported their

Figure 1. Photograph of the International Science
Council(ISC) Members’ Forum in Paris.

activities. Details of this session is available at https://council.science/current/blog/day-3-of-isc-mid-termmeeting/.

Announcement 3:

SCOSTEP Bureau meeting on 11 July 2023
Upcoming Meetings

Kazuo Shiokawa (SCOSTEP President)1 and Keith Groves (SCOSTEP Scientific Secretary)2
1Institute for Space-Earth Environmental Research (ISEE), Nagoya University, Nagoya, Japan
2Boston College, Boston, MA, USA

Kazuo
Shiokawa

AnnouncementThe SCOSTEP Bureau meeting was held at 14001800 CEST on 11 July 2023 at Room: R5 in
CityCube (IUGG venue) in Berlin, Germany and via
online. All Bureau members were attended. The following items were discussed during this meeting.
1. Discussion/Decision Items
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Approval of the minutes of the last Bureau meeting

SCOSTEP/PRESTO Newsletter●Vol. 36●

Keith M.
GrovesUpdates of action items from the last Bureau meeting
Budget status (2022 final; 2023 status; 2024 plan)
Membership Committee report
Application for the new SCOSTEP membership
SCOSTEP Fellow procedures

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Draft agenda of the General Council Meeting

Interview for the STP-16 venue●

Resolution of data exchange across borders in IAGA
and IUGG●

2. Report Items●●

Selection status of new SDRs
Scientific Secretary (SS) Office Updates
Reports from participating bodies (COSPAR, IAGA,
IAMAS, IAU, IUPAP, SCAR, URSI, WDS)

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Updates of ISC, UN_STSC, UN_COPUOS, and
ISWI activities

PRESTO updates
School activities supported by SCOSTEPSCOSTEP online capacity building lectures
SCOSTEP Distinguished Service Award 2023
SCOSTEP Visiting Scholar (SVS) updates

Highlight on Young Scientists●●

Article●WMO-ISES-COSPAR Space Weather ForumSCOSTEP comic book updates

The full report of the Bureau meeting will be opened
from the SCOSTEP website after approval of the Bureau minutes at the next Bureau meeting.

Announcement 4:

SCOSTEP General Council Meeting on 14 July 2023
Kazuo Shiokawa (SCOSTEP President)1 and Keith Groves (SCOSTEP Scientific Secretary)2
1Institute for Space-Earth Environmental Research (ISEE), Nagoya University, Nagoya, Japan
2Boston College, Boston, MA, USA

T

Keith M.
GrovesAwards 2022. Then the SCOSTEP Distinguished Service Award 2023 was given to Dr. Marianna Shepherd
from the President. Then financial matters were explained from Keith Groves, i.e., SCOSTEP closing
statements 2022, SCOSTEP budget details for 2022,
2023, and 2024 (anticipated), and membership fees.
Then, application for the new SCOSTEP membershipfrom Rwanda was discussed. Finally, election of new
SCOSTEP executives for July 2023 – July 2027 weremade by vote. The new President and Vice President
were decided as Dr. Kazuo Shiokawa (continuationfrom the previous term) and Dr. Bernd Funke, respectively. A full copy of the minutes of the General Council
meeting will be put on the SCOSTEP website at: https://
scostep.org/meeting-minutes-archive/.

Upcoming Meetings

he SCOSTEP General Council Meeting was held at
1730-1900 CEST on 14 July 2023 at Room R13 in
CityCube (IUGG venue) in Berlin, Germany and via
online. After the opening remarks and approval of agenda, the minutes of the previous General Council Meeting (25 February 2022) was approved. Then, updates
and status reports on SCOSTEP activities were reported
by Kazuo Shiokawa (President) and Keith Groves(Scientific Secretary), i.e., SCOSTEP leadership updatesof 2022–2023, SCOSTEP membership updates, newScientific Discipline Representatives, Scientific Secretary Office updates, PRESTO Program updates, updatesof ISC, UN_STSC, and UN_COPUOS activities,
SCOSTEP Visiting Scholar (SVS) Program in 20222023, capacity building schools supported by SCOSTEPin 2022-2023, SCOSTEP online capacity building lectures, SCOSTEP comic book updates, and SCOSTEP

Meeting Report

Kazuo
Shiokawa

Announcement

SCOSTEP/PRESTO NewsletterVol. 36

11

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 “scostep_at_bc.edu” or “scosteprequest_at_bc.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
Keith Groves (keith.groves_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:Odele Coddington (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 coleader), Duggirala Pallamraju (Pillar 2 co-leader), Nick Pedatella (Pillar 2 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),
Keith Groves (Scientific Secretary, ex-officio), Mamoru Ishii (WDS), Jorge Chau (URSI),
Kyung-Suk Cho (IAU), Yoshizumi Miyoshi (COSPAR), Renata Lukianova (IAGA/IUGG), Peter
Pilewskie (IAMAS), Pravata Kumar Mohanty (IUPAP), and Lucilla Alfonsi (SCAR)
website: https://scostep.org.

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SCOSTEP/PRESTO NewsletterVol. 36