SCOSTEP/PRESTONEWSLETTER
Vol. 35, April 2023

Inside this issue
Article 1:
SOSMAG – Service
Oriented Spacecraft Magnetometer on GEOKOMPSAT-2A

1

Article 2:
3
Development ofVery Low Frequency(VLF) Radio Wave
Database in Anchor
University for Regional Advancement of SolarTerrestrial Physics
Research
5
Article 3:
Atmospheric Electricity Measurments at the Villum
Research Station
Highlight onYoung Scientists 1:
Patrick Essein /
Ghana

7

Highlight onYoung Scientists 2:
Talwinder Singh /USA

8

Article 1:

SOSMAG – Service Oriented Spacecraft
Magnetometer on GEO-KOMPSAT-2A

David
Fischer

Melanie
Heil

Hans-Ulrich Ovidiu Dragos
Auster Constantinescu

Magda
Delva

Nick
Hatzigeorgiu

WernerMagnesFerdinand
Plaschke

Josef
Wilfinger

Ingo
RichterDavid Fischer1, Melanie Heil2, Hans-Ulrich Auster3, Ovidiu Dragos Constantinescu3, 4, Magda Delva1, Nick Hatzigeorgiu5, Werner Magnes1, Ferdinand Plaschke3, Ingo Richter3 and Josef Wilfinger1
1Space Research Institute, Austrian Academy of Sciences, Graz, Austria
2European Space Agency, Darmstadt, Germany
3Institute for Geophysics and Extraterrestrial Physics, TU Braunschweig, Germany
4Institute for Space Sciences, Bucharest, Romania
5Space Sciences Laboratory, UC Berkeley, USAT

he Service Oriented Spacecraft Magnetometer (SOSMAG) [1] is part of
ESA’s distributed Space Weather Sensor
System (D3S), which has the task to pro-vide accurate information for forecast/
nowcast of space weather to infrastructure or satellite owners [Figure 1].

Upcoming Meetings 9

Figure 1. Impact of Space Weather,©ESA/Science Office,CC BY-SAVol.
3.0 35IGO.
SCOSTEP/PRESTO
Newsletter

S

ArticleOSMAG is a part of the Korean Space Environment
Monitor (KSEM) on the Korean GEO-KOMPSAT2A satellite, which was launched to geostationary orbit(128° E) in December 2018. The measurements of SOSMAG cover the previous gap of geostationary magnetic
field measurements over Eastern Asia and complement
the measurements of the GOES satellites above theAmerican continent.

Highlight on Young Scientists

T

he SOSMAG instrument is designed to operate on asatellite without magnetic cleanliness program andemploys two science-grade fluxgate sensors on a shortboom and two additional anisotropic magnetoresistancesensors within the spacecraft body [Figure 2]. Data
from all four sensors is combined mathematically toattenuate magnetic disturbances from the spacecraft [2].
This combination can be done using on-board or groundprocessing.

Figure 3. SOSMAG Dashboard in the SWE Portal.

Meeting Report

Figure 2. SOSMAG qualification model with a)electronics box, b) boom with carbon fiber based
interface plate, c) two fluxgate sensors mounted onto
the boom and d) two anisotropic magnetoresistancesensors [1].

T
Upcoming Meetings

he processed data from SOSMAG is available at
ESA’s Space Weather Service Network (SWE) [3]after free registration. Data is available with 3 different
delays and qualities:●●●

Announcement
2

Real-time data is provided with a delay of less than
5 minutes. It uses predetermined calibration andcleaning factors.
Preliminary data is provided with a delay of lessthan 2 days. It is still calculated using predeterminedcalibration and cleaning factors, but possible gaps inreal-time transmission and processing are closed.

Final data is provided with a delay of 98 days. Thisdata uses updated calibration and cleaning factors
and provides the highest quality.

AIn exemplary screenshot of the SWE portal isshown in Figure 3. Detailed information about
SOSMAG data and its properties can be found at [4].
n addition to direct retrieval from the SWE portal,
registered SWE users can also use PySPEDAS [5] asutility for data downloading. The SPEDAS team also
provides daily overview plots [see Figure 4] that can becompared with data from magnetospheric missions easily [6].

SCOSTEP/PRESTO NewsletterVol. 35

Figure 4. SPEDAS Summary Plot.

[1] Magnes, W.; Hillenmaier, O.; Auster, H.-U.;
Brown, P.; Kraft, S.; Seon, J.; Delva, M.; et al.
‘Space Weather Magnetometer Aboard GEOKOMPSAT-2A’. Space Science Reviews, 216, 119(2020). https://doi.org/10.1007/s11214-020-007422.
[2] Constantinescu, O. D.; Auster, H.-U.; Delva, M.;
Hillenmaier, O.; Magnes, W.; and Plaschke, F.
‘Principal Component Gradiometer Technique for
Removal of Spacecraft-Generated Disturbancesfrom Magnetic Field Data’. Geoscientific Instru-

[3] https://swe.ssa.esa.int/[5] https://github.com/spedas/pyspedas[6] http://themis.ssl.berkeley.edu/summary.php?
year=2022&month=12&day=01&hour=0024&sum
Type=kompsat&type=sosmag

Articlementation, Methods and Data Systems Discussions, 25 May 2020, 1–26. https://doi.org/10.5194/
gi-2020-10.
[4] https://swe.ssa.esa.int/sosmag

Highlight on Young Scientists

Article 2:

Development of Very Low Frequency (VLF) Radio Wave
Database in Anchor University for Regional Advancement of Solar-Terrestrial Physics Research

Victor U. J. Nwankwo1
1Centre for Space Research (CESPAR), Anchor University, Lagos, Nigeria

he Earth’s atmosphere is dynamic and complex,
characterised by temporal and spatial variability andsignificantly varies with time and location. This scenario
makes multiregional deployment of scientific observational facilities (for atmospheric data acquisition) imperative, for better coverage and remote sensing of regionsof interest. While the effort of many institutions in Africa is acknowledged in this regard, it is still worrisomethat most parts of Africa (including Nigeria) lack adequate deployment of ground-based and space-borne observational facilities. Data shows that our regions are
not well represented in the ongoing effort by the World
Archive of Low-frequency data and observation(WALDO), and a limited or absence of global GNSS
and digital ionosonde ground sites in most regions (seeFig 1). This underscores the need to embark on global
deployment of more facilities and upgrade of the existing ones for a wider coverage, especially in the African
continent [1].

Meeting Report

T

Victor U. J.
NwankwoUpcoming Meetings

I

Announcementn 2018, Anchor University, Lagos (AUL) establishedthe Space, Atmospheric Physics and Radio Wave
Propagation Laboratory (AUL Space Lab) to (among
other objectives) address the dearth of research data in
our region through deployment of ground-based observational facilities and subsequently building regional
and institutional database for advancing research in solar-terrestrial Physics, science and technology [4]. At
inception, the AUL Space laboratory was a makeshift
cubicle carved out of the Departmental office of Physics
programme and housed the data capturing equipmentwith very limited space for researchers.

D
Figure 1. (a) Map of Global GNSS ground-based sites
used for processing total electron content (TEC) data[2] (b) VLF sites with data on or in queue fromWALDO (Adapted from www.waldo.world) and (c)Sites for digital ionosonde sounding system (DISS),
Next generation ionosonde (NEXION), scintillation
network decision aid (SCINDA) [3].

ata acquisition effectively began in 2019 using a
multichannel very low frequency (VLF) radio
waves Receiver (donated to the laboratory by the IndianCentre for Space Physics (ICSP) and Weather Station(measuring meteorological parameters). The VLF Receiver recorded time-variant amplitude of VLF radio
waves from 4 transmitters at the time, including HWU(France), NWC (Australia), JJI (Japan) and VTX (India)(Fig 2). As the data accumulated over time, we saw the
obvious need to properly process, store and subsequent-

SCOSTEP/PRESTO NewsletterVol. 353

Articlely retrieve the already acquired data, as well as makeprovision for a real-time data catalogue that will be publicly available for researchers and stakeholders in thefield.

Highlight on Young Scientists
Meeting Reporthile this effort lasted, we experienced intervals ofdata gaps mainly due to moments of technicalhitches and power outage, and eventual breakdown of
the antenna of the only receiver at the time. It was on
this premise that we successfully applied to the 2021
Scientific Committee on Solar-Terrestrial Physics(SCOSTEP)/PRESTO Grant for creating database ofsolar-terrestrial data. We effectively utilized the grant tosignificantly progress and expand our laboratory to thecapacity where we are now well-placed to pursue andmeet the sole objectives of the laboratory. The outcome
and/or product of the project include a successful archiving of VLF radio wave amplitude data that is now
available for SCOSTEP community and other researchers on www.cespar.space (see webpage overview in Fig3), and the acquisition of new VLF receivers that enabled us to resume data acquisition after a long break.

T

he impacts of the completed project include (i) better equipment and expansion of the recipient laboratory (AUL Space Lab), (ii) enhanced capacity to provide students and scholars with training and mentorshipin solar-terrestrial physics (iii) upgrade of the recipientlaboratory to Anchor University Center for Space Research (CESPER, see Fig 4) and (iv) increased visibility
leading to scientific cooperation and/or collaboration
with more institutions (more details in [4]).

Figure 2. Signal propagation paths and associated data
received at AUL Space Lab.

Upcoming Meetings
Announcement
4W

Figure 4. (a) AUL Space Lab at inception (b & c) AUL
Space Lab upgraded to Centre for Space Research(CESPAR).

A
Figure 3. An overview of AUL Space Lab and
CESPAR homepage at www.aulspacelab.space andwww.cespar.space.

SCOSTEP/PRESTO NewsletterVol. 35

cknowledgement: The AUL Space Lab teamacknowledge and thank SCOSTEP and its management team for the SCOSTEP/PRESTO Grant that supported our effort. The following are also highly
acknowledged for their unflinching support that madethis achievement possible: The Vice Chancellor, Prof.
Samuel O. Bamdele and members of Anchor University
Management Team, the Dean of Faculty of Natural,
Applied and Health Sciences (FNAHS), the AUL SpaceLab Technical Crew, the Department of Physics(Anchor University), Prof. William Denig (SJCM,USA), Prof. S. K. Chakrabarti (ICSP, India), Prof. J-P

References:

3. OFCMS Report, 2013. Report on space weather observing systems: current capabilities and requirements for next decade. NSWPC Joint Action Groupfor Space Environment Gap Analysis, USA.
4. CESPAR, 2022. Our Journey to Space, ValuePlus
Inc., Lagos, Nigeria, https://www.cespar.space/doc/bulletin.pdf.

Highlight on Young Scientists

1. Nwankwo et al., 2020. Radio aeronomy in Nigeria:First results from very low frequency (VLF) radio
waves receiving station at Anchor University, Lagos.
2020 IEEE-ICMCECS, Lagos, Nigeria, DOI:
10.1109/ICMCECS47690.2020.247002.

2. Verkhoglyadova et al., (2016). Solar wind driving of
ionosphere-thermosphere responses in three storms
near St. Patrick’s Day in 2012, 2013, and 2015. J.
Geophy. Res.: Space Physics, 121 (9), 8900-8923.

ArticleRaulin (CRAAM, Brazil), Prof. Caitriona Jackman andProf. Peter Gallagher of DIAS, Ireland (DIAS Dunsink
Observatory recently donated a Raspberry Pi magnetometer and VLF Receiver to support our effort), Prof
O.O. Akinwnmi (AUL, Nigeria), Dr. O.E. Abe (Federal
University, Oye Ekiti, Nigeria) and other colleagues too
numerous to mention here.

Article 3:

Atmospheric Electricity Measurments at the Villum Research StationCTheight with diurnal variations of GEC (Harrison andAmbaum 2013; Nicoll and Harrison 2016; Harrison etal. 2020). However, an experimental confirmation of
charge-cloud interactions is a challenging task, because
it requires quality-controlled concurrent measurementsof GEC and cloud properties in fair-weather conditions
not only at the surface but in clouds as well.

In August 2022, we installed a Chilworth JCI 131electric field mill at the Villum Research Station(VRS) at Station Nord/Greenland (81.36 N, see Picture1) to provide continuous measurements of potential gradient at ground level to characterize GEC variations.
Our measurements will be part of the global atmospheric electricity monitoring network for climate and geophysical research (Nicoll et al. 2019). The station is also
equipped with a Vaisala CL51 ceilometer, which gives
information about overlaying layers of clouds and aerosols and an Airel NAIS aerosol spectrometer, whichmeasures the mobility distribution of the ions. Different
radiometers (e.g pyranometer) will allow us to quantify
charge-cloud signatures on the surface energy budget.
The particular meteorological conditions (e.g. negligible
diurnal variability during polar night) that facilitate excellent GEC measurements and the frequent presence ofliquid-phase layered clouds, make VRS an ideal location to study charge-cloud processes and their climatic
signature (Harrison and Nicoll 2018). Observational
results will ultimately improve the parameterization andrefine the modeling of GEC-related processes.

SCOSTEP/PRESTO NewsletterVol. 35

Announcement

heory suggests that current-flow through a stratiform cloud will cause accumulation of space charge
on the cloud edges, with charge transferred to cloud
droplets and aerosol particles, with potential influenceson cloud microphysics that in turn may affect cloud
droplet size distributions, precipitation, lifetime, andradiative properties. If this is the case, it is reasonable toassume that charge-cloud processes cause tangible
changes in atmospheric thermal stratification and radiation and as a consequence on the entire energy budget.
Recent progress has provided some observational evidence for charge effects on clouds, relating cloud-base

Stergios Misios

Upcoming Meetings

louds play a vital role on weather and climate, affecting precipitation and Earth’s radiation budget.
Nonetheless, the processes that govern their microphysical properties and feedbacks are far from understood.
The majority of observational and all climate modellingstudies assume a neutral environment, when studying
cloud variations and cloud-aerosol interactions, hence
neglecting altogether one key property of the atmosphere: electric charges. High energy cosmic rays of galactic and solar origin, natural radioactivity, lighting inthunderstorms and electrified shower clouds, produce
ion clusters and charge the whole atmosphere causing aubiquitous potential difference between the ionosphereand the surface (Williams and Mareev 2014). This
Global Electric Circuit (GEC) allows the flow of charges to the surface in the fair-weather (undisturbed) regions of the globe.

Meeting Report

Stergios Misios1
1National Observatory of Athens, Athens, Greece

5Article

the NCSR Demokritos ACTRIS station, Mt Helmos,
Greece (2315 m asl) during the winter 2021/2022.

Highlight on Young Scientists
Meeting Report
Upcoming Meetings
Announcement
6

Picture 1. The Chilworth JCI 131 next to the Flygers
hut, Greenland.

Figure 1 shows raw hourly Potential Gradient timeseries at the VRS for August 2022. The mean PG isabout 69 V/m and is enhanced considerably duringsnowstorms. As there is no direct communication to the
instrument, the data are retrieved infrequently, every
time scientists visit VRS, with the latest checkout in
Dec 2022.

The
project(https://isaaffik.org/projects/view/atmospheric-electricity-measurments-at-the-villumresearch-station?iri=%2Fapi%2Fprojects%2F20b6ba8626e5-43f5-8651-552d2d3e5801) brings together expertise in space-climate (Physics, Astronomy and Geoscience, Uni. Aarhus), aerosol and clouds theory andmeasurements at VRS (Env. Science, Uni. Aarhus),
atmospheric electricity measurements, instrumentationand modeling (National Observatory of Athens, Greece)
to assess the climatic relevance of GEC through influencing layered clouds. The JCI-131 has been purchasedby the Villum Experiment project “Environmental consequences of solar cosmic rays ” and is planned to operate at VRS for 2 years at least. We acknowledge the
SCOSTEP-PRESTO Grant for campaigns and Marie
Skłodowska-Curie Action “Electric Volcano” for thefinancial support to visit VRS and the testing phase at
Mt. Helmos. Scientific and logistic support at different
stages of the project was given by: J. Skafte, K. Mortensen, M.F. Knudsen, Aarhus, K. Eleftheriadis and P. Fetfatzis NCSR Demokritos, A. Gourzelas, V. Daskalopoulou, G. Katoufas, V. Amiridis.
Refecences:
Harrison, R. G., and K. A. Nicoll. 2018. 'Fair weather
criteria for atmospheric electricity measurements', Journal of Atmospheric and Solar-Terrestrial Physics, 179:
239-50.
Harrison, R. Giles, and Maarten H. P. Ambaum. 2013.
'Electrical signature in polar night cloud base variations', Environmental Research Letters, 8: 015027.

Harrison, R. Giles, Keri A. Nicoll, Evgeny Mareev, Nikolay Slyunyaev, and Michael J. Rycroft. 2020.
'Extensive layer clouds in the global electric circuit:their effects on vertical charge distribution and storage',
Proceedings of the Royal Society A: Mathematical,
Physical and Engineering Sciences, 476: 20190758.

Figure 1. Potential gradient time series for August2022. Cyan box shows a power failure. Peaks of PG
correspond to snowstorms.

One key challenge in operating an instrument in theharsh Arctic environment is the heat insulation toprevent ice build up. The JCI-131 is particularly prone
to environmental conditions because of the rotatingplate, which can break when ice accumulates at the headin the case of long power failures (Our instrument broke
during the testing phase). We have isolated the instrument with two flexible silicon heating pads and theirperformance was examined by taking measurements at

SCOSTEP/PRESTO NewsletterVol. 35

Nicoll, K. A., and R. G. Harrison. 2016. 'Stratiform
cloud electrification: comparison of theory with multiple in-cloud measurements', Quarterly Journal of theRoyal Meteorological Society, 142: 2679-91.
Nicoll, K. A., R. G. Harrison, V. Barta, J. Bor, R. Brugge, A. Chillingarian, J. Chum, A. K. Georgoulias, A.
Guha, K. Kourtidis, M. Kubicki, E. Mareev, J. Matthews, H. Mkrtchyan, A. Odzimek, J. P. Raulin, D.
Robert, H. G. Silva, J. Tacza, Y. Yair, and R. Yaniv.
2019. 'A global atmospheric electricity monitoring network for climate and geophysical research', Journal of
Atmospheric and Solar-Terrestrial Physics, 184: 18-29.
Williams, Earle, and Eugene Mareev. 2014. 'Recent
progress on the global electrical circuit', AtmosphericResearch, 135-136: 208-27.

Article

Highlight on Young Scientists 1:

Ionospheric Plasma Fluctuation Response to Space Weather
events over the Equatorial and Low Latitude Region

IntroductionAs space technology becomes increasingly vital in
our contemporary lives, we become more susceptible to space weather changes and interactions. The
availability and application of these technologies are
therefore influenced by ionospheric "weather," and theprediction of ionospheric conditions continues to bechallenging because of limitations in the consistent observations of key parameters including plasma fluctuations (Essien et al., 2021).

Highlight on Young Scientists

Patrick Essein1, Francis Nkrumah1 and Moses Jojo Eghan1
1University of Cape Coast, Department of Physics, Cape Coast, Ghana

Patrick Essein

309.5o. Consistent observation on the September 2017
and August 2008 storms revealed the ionospheric plasma fluctuations.

It is obvious that the characteristics of the ionosphericfluctuations observed during the storm day and recovery phase days are similar to the MSTIDs observed byFigueirido et al. (2018) and Essien et al. (2021) in theequatorial and low latitude region.

O

Meeting Reportn the 17th of March 2015, a strong (~50 nT) compression occurred, indicative of a shock reaching
the magnetosphere, resulting geomagnetic storm with anindex of -223 nT, indicating the generation of a strong
ring current followed by a slow, long-lasting ring current during the recovery phase.

W

Figure 2. Keograms created from the series dTEC
maps on March 17th, 2015; longitudinal (top) and latitudinal (bottom). The black dashed lines indicate thedawn and dusk solar terminator.

Upcoming Meetingse estimated the detrended Total Electronic Content (dTEC) using data from GNSS receivers(Otsuka et al., 2013, Figueiredo et al., 2018, Essien etal., 2021). Figure 1 shows the dTEC profile of GPS
PRN 23 observed by a receiver in Accra (5.60° N, 0.19°
W). There are fluctuations between 08:00 and 09:30
UT, and the intensity gradually reduced.

Reference:
1. Essien, P., et al., (2021). Long-term study on
MSTIDs observed over the South American Equatorial Region. Atmosphere, 12(11), 1409.
Figure 1. dTEC profile over Accra on 17th March2015.

eries of dTEC maps of South American regions
were used to create keograms as shown in Figure 3.
The wavelength, period, phase velocity and propagation
direction are 633.5 km, 34.5 min, 306.0 m/s, and3. Otsuka, et al., (2013). GPS observations of MSTIDs
over Europe. In Annales Geophysicae (Vol. 31, No.
2, pp. 163-172). Copernicus GmbH.

Announcement

S

2. Figueiredo, et al., 2018 MSTIDs observed by dTEC
maps over Brazil. Journal of Geophysical Research:
Space Physics, 123, 2215–2227.

SCOSTEP/PRESTO NewsletterVol. 357

Highlight on Young Scientists 2:

ArticleImproving the Arrival Time Estimates of Coronal Mass Ejections by Using Magnetohydrodynamic Ensemble Modeling,
Heliospheric Imager data, and Machine Learning

Highlight on Young Scientists

Talwinder Singh1
1University of Alabama in Huntsville, Huntsville, AL, USAT

he arrival time prediction of Coronal mass ejections(CMEs) is an area of active research. Many methods
with varying levels of complexity have been developed to
predict CME arrival. However, the mean absolute error(MAE) of predictions remains above 12 hours, even with
the increasing complexity of methods.

W

Meeting Reporte have developed a new method for CME arrival
time prediction that uses magnetohydrodynamic
simulations involving data-constrained flux-rope-based
CMEs, which are introduced in a data-driven solar windbackground (Singh et al., 2023). The CME model was explained in detail in Singh at al. (2022.) We found that, for 6
CMEs we studied, the MAE in arrival time was ~8 hours.

W

e further managed to improve our arrival time predictions by using ensemble modeling and comparing
the ensemble solutions with STEREO-A&B heliospheric
imager data. This was done by using our simulations to

TalwinderSinghcreate synthetic J-maps and comparing them with J-maps
created from HI observations (See Figure 1). Two machinelearning (ML) methods, the lasso regression and (LR) neural networks (NNs), were used for this comparison. Using
LR, we could reduce the MAE to ~4 hours. NNs made it
possible to reduce the MAE to ~5 hours for the cases when
HI data from both STEREO-A&B were available. Interestingly, NNs can provide similar MAE when only the STEREO-A data is used, which is encouraging since only STEREO B is currently not operational. Our methods also resulted in very encouraging values of standard deviation(precision) of arrival time.

O

ur methods demonstrate significant improvements in
the CME arrival time predictions. Our work highlights
the importance of using ML techniques in combination
with data-constrained magnetohydrodynamic modeling to
improve space weather predictions.

Upcoming Meetings
Announcement

Figure 1. Left panels: J-maps created using HI1 and HI2 data from STEREO-A (top) and STEREO-B (bottom)
showing the 12 July 2012 CME. The tracked CME front is shown with red symbols in both J-maps. Middle panels: Synthetic J-maps created from the simulation of the seed ensemble member for the 12 July 2012 CME fromSTEREO-A (top) and STEREO-B (bottom) vantage point. The CME front is traced with the blue line. Right panels: The time-elongation data extracted from the J-maps by tracing the CME fronts in observed J-map (black line)
and synthetic J-maps for all ensemble members (colored according to the travel time in hours from eruption to
Earth impact). The top panel is for STEREO-A and the bottom panel is for STEREO-B.
References:

Singh, T., Kim, T. K., Pogorelov, N. V., and Arge, C. N.

8SCOSTEP/PRESTO NewsletterVol. 35(2022). Ensemble simulations of the 2012 July 12 coronalmass ejection with the constant-turn flux rope model. The
Astrophysical Journal, 933(2):123.

by Using Magneto- hydrodynamic Ensemble Modeling,
Heliospheric Imager data, and Machine Learning. arXiv eprints, page arXiv:2302.05588.

ArticleSingh, T., Benson, B., Raza, S. A. Z., Kim, T. K., Pogorelov, N. V., Smith, W. P., and Arge, C. N. (2023). Improving the Arrival Time Estimates of Coronal Mass Ejections

Upcoming meetings related to SCOSTEP
LocationContact Information

PRESTO Workshop & School

May 29-Jun. 2,
2023

Trieste, Italy

https://indico.ictp.it/event/10176

The 16th Hellenic Astronomical Conference

Jun. 25-28, 2023

Athens, Greece

https://helas.gr/conf/2023/

IUGG 2023

Jul. 11-20, 2023

Berlin, Germany

https://www.iugg2023berlin.org/

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/

International Conference on Space weather
Aug. 21-23, 2023
and Technology Applications

Lusaka, Zambia

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

Sep. 4-8, 2023

Ilorin, Nigeria

Multi-instrumental and model investigationof the high-speed solar wind streams effecton the coupled ionosphere-plasmaspheresystemOctober, 2023

Prague, Czech Republic

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

Oct. 2-6, 2023

Arua, Uganda

The 2023 Sun-Climate Symposium

Oct. 16-20, 2023

Flagstaff, AZ, USA

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

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 https://www.iau.org/science/
Africameetings/future/symposia/

11th SCAR Open Science Conference

Aug. 19-23, 2024

Pucon, Chile

Meeting Report

Date

Highlight on Young Scientists

Conference

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

Announcement

Vol. 35

Upcoming Meetings

SCOSTEP/PRESTO Newsletter

9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. 35