SCOSTEP/PRESTONEWSLETTER
Vol. 33, October 2022

Inside this issue
Article 1:
A new journey ofthe Arase satellite
to the 25th solar
cycle

1

Article 2:
NASA's Moon to
Mars Space Weather Analysis Office3

Highlight onYoung Scientists 1:
Jing Liu / China

5

Article 1:

A new journey of the Arase satellite to
the 25th solar cycle
Yoshizumi Miyoshi1 and Iku Shinohara2
1Institute for Space-Earth Environmental Research, Nagoya University, Nagoya,Japan
2Space and Planetary Research Group, ISAS, JAXA, Sagamihara, Japan

Highlight on
6Young Scientists 2:
Harneet Kaur Sangha / USA

Yoshizumi
MiyoshiThe geospace explanation satellite
Arase (ERG) was launched in December 2016 and has observed since
March 2017 [1] (Figure 1). The five

Iku Shinohara

years of observations covered the transition period from the declining phase of
the 24th solar cycle to the beginningphase of the 25th solar cycle (Figure 2).

Upcoming Meetings 7

Figure 1. Conceptual image of Arase (ERG) satellite in the inner magnetosphere(copyright: ERG Science Team).

SCOSTEP/PRESTO NewsletterVol. 33

Article
Highlight on Young Scientists
Meeting Report
Upcoming Meetings
Announcement
2

Figure 2. (left) Spatial distributions of 2 MeV electrons from the Arase satellite. (right) Long term variations of 2
MeV electrons and sunspot number.

During this period, the Arase satellite revealed many
interesting phenomena in the inner magnetosphere andthe radiation belts. Especially, the Arase satellite has
shed light on the importance of cross-energy coupling
via non-linear wave-particle interactions to cause variations of enhancement and loss of energetic electrons andions. The Arase satellite discovered that electrons arescattered into the loss cone due to chorus-wave particle
interactions and resultant pulsating aurora [2, 3]. The
Arase observed the rapid acceleration of electrons by
non-linear chorus-wave particle interactions [4, 5].
Identifications of energy transfer between waves andparticles are achieved by direct measurements of dot
product between velocity vector v and electric field E ofwaves [6, 7]. And high-energy electron precipitations
and resultant ozone destructions are observed by Arase
and EISCAT coordinated observations [8]. Moreover,many international collaborations with NASA/Van Allen Probes and other satellites, and ground-based observations were realized [9]. All data from the Arase satellite are publicly available from the Center for Heliospspheric Science (https://ergsc.isee.nagoya-u.ac.jp/
index.shtml.en).

V

ery recently, the project has undergone a mission
extension review by JAXA, and the extension has
been approved until the end of FY2032. The extended
mission contributes to comprehensive observations of
the inner magnetosphere and dynamics of the radiation
belts by observations of the whole cycle 25. On the other hand, no large magnetic storms have been observed
during this period. In the upcoming cycle, we expect tohave more opportunities to encounter large geospacestorms during the 25th solar cycle and to observe thedrastic change of geospace. It is well known that geospace shows different variations depending on the largescale structure of the solar wind, for example, CME and
CIRs, which occurrence depends on the solar cycle. The
Arase satellite will conduct observations over the solar
cycle to clarify the solar wind-magnetosphere interaction by observing the different types of geospacestorms. Furthermore, it will play a role in international
geospace exploration by collaborating with groundbased observations such as EISCAT_3D, and by conducting joint observations with other satellites/ground-

SCOSTEP/PRESTO NewsletterVol. 33

based observations. We look forward to the Arase mission for the cycle 25 and collaboration with SCOSTEP
colleagues.
References:[1] Miyoshi, Y., Geospace Exploration Project ERG,
Earth Planets Space, 70:101, doi:10.1186/s40623-0180862-0, 2018.
[2] Kurita et al., Deformation of electron pitch angle
distributions caused by upper-band chorus observed by
the Arase satellite, Geophys. Res. Lett., 45,
doi:10.1029/2018GL079104, 2018.
[3] Saito et al., Data-driven simulation of rapid flux
enhancement of energetic electrons with an upper-band
whistler burst, J. Geophys. Res., 126, e2020JA028979,
doi:10.1029/2020JA028979, 2021.
[4] Kasahara et al., Pulsating aurora from electron scattering by chorus waves, Nature, 554, 337-340,
doi:10.1038/nature25505, 2018.
[5] Hosokawa, K., Multiple time-scale beats in aurora:
precise orchestration via magnetospehric chorus waves,
Scientific Reports, 10, 3380, doi:10.1038/s41598-02059642, 8, 2020.,[6] Shoji, M., Discovery of proton hill in the phasespace during interactions between ions and electromagnetic ion cyclotron waves, Scientific Reports, 11:13480,
doi:10.1038/s41598-021-92641-0, 2021.

[7] Asamura, K., Cross-energy couplings from magnetosonic waves to electromagnetic ion cyclotron waves
through cold ion heating inside the plasmasphere, Phys.
Rev.
Lett.,
127,
25101,
doi:10.1103/
PhysRevLett.127.245101, 2021.
[8] Miyoshi, Y. et al. Penetration of MeV electrons into
the mesosphere accompanying pulsating aurorae, Scientific Reports, 11, 13724, doi:10.1038/s41598-021-92611-3, 2021.
[9] Miyoshi, Y. et al. Collaborative Research Activitiesof the Arase and Van Allen Probes, Space Sci Rev, 218,
38, doi:10.1007/s11214-022-00885-4, 2022.

Article

Article 2:

NASA's Moon to Mars Space Weather Analysis Officepace weather, mostly driven by our Sun's activity,
can result in solar storms that cause damage to oursatellite's instruments, interfere with GPS signals andcommunication systems, and even disrupt power grids.
An important consideration for human deep space exploration missions is the hazardous radiation environment created by the effects of space weather that can
impact astronaut safety. As NASA plans for missions
beyond Low-Earth Orbit (LEO), there is a need to improve space weather environment modeling capabilities,
real-time space weather data analysis, and assessmentsof radiation risks and how these can be communicatedto the crew. NASA's Space Radiation Analysis Group(SRAG) supports the US crew members aboard the International Space Station (ISS). SRAG monitors andoperates a console that includes analysis of satellite imagery and energetic charged particle measurements. Dueto the mid-inclination LEO orbit of the ISS, crews
aboard the ISS are protected from ionizing radiation by
Earth's magnetic field most of the time. As NASA's human spaceflight goals extend beyond LEO, astronauts
will experience a more hazardous environment. These

Meeting Report

S

Highlight on Young Scientists

Yaireska Collado-Vega1, Anna Chulaki1,2, Robert Loper1,2, Michelangelo Romano1,2, Carina
Alden1,2, Mary Keenan1,3, Mary Aronne1,2, Mattie Anastopulos1,2, Chris Stubenrauch1,2, andHannah Hermann1,2
1NASA Goddard Space Flight Center, Greenbelt, MD, USA
2Catholic University of America, Washington, DC, USA
3ADNET SYSTEMS INC., Bethesda, MD, USA

Upcoming Meetings
Announcement

Figure 1. Yaireska (Yari) Collado-Vega (left-M2M Director) discussing an analysis with Anna Chulaki (rightM2M Deputy Director).

SCOSTEP/PRESTO NewsletterVol. 333

Article
Highlight on Young Scientists

Figure 2. CCMC-SRA-M2M Collaboration - NASA's in house R2OO2R pipeline for human space exploration.
Credit: CCMC.

future missions will be flying in deep space and will nolonger have the Earth’s protective magnetic field shielding them from the ionizing radiation associated withsolar storms.

I
Meeting Reportn 2018, NASA SRAG started a collaboration with theCommunity Coordinated Modeling Center (CCMC)
to transition solar energetic particle (SEP) models fromthe research community into a platform that could be
used operationally to support upcoming space missions.
The CCMC developed a tailored version of their SEP
Scoreboard concept and needed an organization to support the testing and evaluation of this application in asemi-operational setting. To address this need, theMoon to Mars (M2M) Space Weather Analysis Office
was established to support NASA’s SRAG with humanspace exploration activities by providing novel capabili-

Upcoming Meetings
Announcement
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SCOSTEP/PRESTO NewsletterVol. 33

ties to characterize the space radiation environment.
M2M will work as the proving grounds and testbed forcapabilities that can eventually be transitioned to operational agencies. M2M also supports NASA robotic missions with space weather assessments and anomaly
analysis. To support the transition of models from research to operations, the M2M Office will conduct anevent-based validation in which the real-time model
outputs for specific events of interest (e.g., SPEs/ESPEs
or ICME arrivals) are evaluated. This is a crucial stepto assess model accuracy and performance in a real-time
operational setting. The M2M Office will employ
NASA-specific operational model execution, data products, and displays to leverage capabilities developed incollaboration with CCMC, SRAG, and the broader research community.

Article

Highlight on Young Scientists 1:

The Latitudinal and Inter-Hemispheric Variations of the
Ionospheric Semi-diurnal Lunitidal Perturbations during
the Sudden Stratospheric Warming eventTIn addition to the longitudinal differences of the semidiurnal lunitidal (M2) perturbations in the low latitude (Liu et al., 2019), my recent studies focused on thelatitudinal and inter-hemispheric variations of the ionospheric M2 perturbations during the SSW. We mainly
used the ground-based vertical total electron content

Jing Liu(TEC) data, either from the Madrigal database or calculated from the Global Navigation Satellite System(GNSS) data. The amplitude and phase of different
wave components were extracted with harmonic analysis.

F

igure 1 shows the TEC M2 amplitude (A M2) variations during SSW events as a function of cumulativedays and geomagnetic latitudes. It shows that TEC M2
perturbations enhance around the SSW peak temperature. A M2 peaks around the crest regions of the Equatorial Ionization Anomaly and the northern A M2 crests arecloser to the geomagnetic equator than the southern
ones. We suggest wind effect on the equatorial plasma
fountain may be a key contributor to this characteristic.
In addition, clear A M2 enhancements extend to middle
latitudes only in the Southern Hemisphere. Meanwhile,
there are also longitudinal differences in the A M2 magnitude and in the M2 manifestation in the southern middle
latitude. For detailed results and discussions, please refer to our papers (Liu et al., 2021, 2022a, 2022b).

Meeting Report

he SSW event is a polar stratospheric phenomenon
caused by the breakdown of the polar vortex due toits interaction with the enhanced planetary wave
(Matsuno, 1971). During the SSW, the ionosphere wasreported to experience characteristic perturbations(Goncharenko & Zhang, 2008; Pedatella et al., 2018).
Studies on the unexpected SSW-ionosphere relationshipgreatly benefit our understanding of the lower atmosphere-ionosphere coupling. Nevertheless, the manifestation and mechanism of such characteristic perturbations
are not thoroughly documented and understood. Most
previous related studies focused on the low-latitude andthere lacks comprehensive pole-to-pole observations(Goncharenko et al., 2022).

Highlight on Young Scientists

Jing Liu1
1School of Earth and Space Science, Peking University, Beijing, China

Upcoming Meetings
Announcement

Figure 1. The TEC M2 amplitude variations during the 2009 (left) and 2021 (right) SSW events as a function of
cumulative days and geomagnetic latitudes. The horizontal dashed lines represent the geomagnetic equator. The
vertical dashed lines mark the occurrence of the SSW peak temperature.

SCOSTEP/PRESTO NewsletterVol. 335

References:

ArticleGoncharenko, L., & Zhang, S. (2008). Ionospheric signatures of sudden stratospheric warming: Ion temperature at middle latitude. Geophysical Research Letters,
35(21), L15804. https://doi.org/10.1029/2008gl035684.

Highlight on Young Scientists
Meeting Report
Upcoming Meetings
Announcement
6

Goncharenko, L. P., Harvey, V. L., Randall, C. E., Coster, A. J., Zhang, S.-R., Zalizovski, A., et al. (2022).
ObservationsofPole-to-Pole,
Stratosphere-toIonosphere Connection. Frontiers in Astronomy andSpace Sciences, 8, 768629. https://doi.org/10.3389/
fspas.2021.768629.
Matsuno, T. (1971). A Dynamical Model of the Stratospheric Sudden Warming. Journal of the Atmospheric
Sciences,
28(8),
1479–1494.
https://
doi.org/10.1175/1520-0469(1971)028<1479:admots>2.0.co;2.

Pedatella, N., Chau, J., Schmidt, H., Goncharenko, L.,
Stolle, C., Hocke, K., et al. (2018). How Sudden Stratospheric Warming Affects the Whole Atmosphere. Eos,
99. https://doi.org/10.1029/2018eo092441.
Liu, J., Zhang, D. -H., Hao, Y. -Q., & Xiao, Z. (2019).
The comparison of lunar tidal characteristics in the lowlatitudinal ionosphere between East Asian and Ameri-can sectors during stratospheric sudden warming events:
2009-2018. Journal of Geophysical Research: Space
Physics. https://doi.org/10.1029/2019ja026722.
Liu, J., Zhang, D., Goncharenko, L. P., Zhang, S., He,
M., Hao, Y., & Xiao, Z. (2021). The latitudinal variation and hemispheric asymmetry of the ionospheric lunitidal signatures in the American sector during major
Sudden Stratospheric Warming events. Journal of GeophysicalResearch:Space
Physics.
https://
doi.org/10.1029/2020ja028859.
Liu, J., Zhang, D., Sun, S., Hao, Y., & Xiao, Z. (2022a).
Latitudinal and interhemispheric differences of the ionospheric semi-diurnal lunitidal perturbations during the2009 Arctic sudden stratospheric warming event in theeastern Asia–Australia sector. Earth, Planets and Space,74(1), 22. https://doi.org/10.1186/s40623-022-01581-x.
Liu, J., Zhang, D., Sun, S., Hao, Y., & Xiao, Z. (2022b).
Ionospheric semi-diurnal lunitidal perturbations during
the 2021 Sudden Stratospheric Warming event: Latitudinal and inter-hemispheric variations in the American,
Asian-Australian, and African-European sectors. Journal of Geophysical Research: Space Physics. https://doi.org/10.1029/2022ja030313.

Highlight on Young Scientists 2:

An Analysis of Bifurcating Region 2 Field-Aligned Currents Using
AMPERE

Harneet Kaur Sangha1
1University of Alabama in Huntsville, Huntsville, AL, USA

T

I

U

T

he Earth system has a number of different components coupled together, influencing one another as
they change. Field-aligned currents connect different
regions of the solar wind-magnetosphere-ionosphereatmosphere system and therefore provide a valuablewindow to view changes occurring within these linked
regions. Iijima and Potemra (1978) were the first to
identify the average structure of the FACs and show tworings of current, one poleward and one equatorward,
termed the Region 1 (R1) and Region 2 (R2) currents,
respectively.
sing the Active Magnetosphere and Planetary Electrodynamics Response Experiment (AMPERE) to
study the FACs, we identified a novel phenomenon previously unseen in this dataset, which we denoted Region
2 Bifurcations (R2Bs). This event can be seen in Figure
1. Figure 1 shows a series of AMPERE polar plots from
2 June 2011, initially presented by Sangha et al. (2020)and followed up by Sangha et al. (2022).

SCOSTEP/PRESTO NewsletterVol. 33

Harneet KaurSanghan the first panel, the standard R1/R2 FAC pattern isevident. As time moves on, the FACs move poleward
indicating a contracting polar cap. At 07:44, both thedawn and dusk R2 FACs are showing a secondary peakin the FAC density, approximately between 02 to 09
MLT and 12 MLT to 20 MLT. By 08:06, these secondary peaks have begun bifurcating from the original R2
FACs (indicated by the arrows), and at 08:12 the duskside R2 current has entirely disconnected from the original.
his example clearly shows the creation and development of an R2B in both the dawn and dusk regions simultaneously. This is rare as this event is predominantly seen at dusk. We suggest there is a relationship between R2Bs and Sub-Auroral Polarization
Streams (SAPS), and substorms. These connections are
explored further by Sangha et al. (2020) and Sangha etal. (2022).

Article
Highlight on Young Scientists

Figure 1. Eight AMPERE polar plots from Sangha et al. (2020) showing the northern hemisphere field-aligned
current densities as a FAC bifurcation event develops. The data are from 06:50 to 08:12 UT on 2 June 2011. Upward FACs are shown in red and downward FACs in blue, with the color scale saturating at ±0.5 μA m−2. The
gray concentric rings show the colatitude to 35°. 12 MLT is at the top of the panels, 06 MLT on the right. The
dashed box indicates the dawn-dusk axis, and the R2B occurrences are shown with the black arrows in panel
08:06 (Sangha et al,. 2020).

References:

Sangha, H., Milan, S. E., Carter, J. A., Fogg, A. R., Anderson, B. J., Korth, H., et al. (2020). Bifurcated Region

Sangha, H. K., Milan, S. E., Anderson, B. J., & Korth,
H. (2022) Statistical Analysis of Bifurcating Region 2
Field-Aligned Currents Using AMPERE. Front. Astron.
Space Sci. 9:731925. doi:10.3389/fspas.2022.731925.

Meeting Report

Iijima, T., & Potemra, T. A. (1978). Large-scale characteristics of field-aligned currents associated with substorms. Journal of Geophysical Research, 83(A2), 599–
615.

2 Field-Aligned Currents Associated with Substorms. J.
Geophys. Res. Space Phys. 125, e2019JA027041.
doi:10.1029/2019JA027041

Upcoming meetings related to SCOSTEP
Conference

Contact Information

Summer Space Weather School- Physics and use of tools

In October, 2022

Houphouët Boigny
University, Abidjan, Côte d’Ivoire

The 1st VERSIM school

Nov. 5-6, 2022

Sodankylä, Finland

https://www.sgo.fi/Events/
VERSIM/

The 10th VERSIM Workshop

Nov. 7-11, 2022

Sodankylä, Finland

https://www.sgo.fi/Events/
VERSIM/

International Workshop on Machine Learning for Space Weather: Fundamentals, Tools Nov. 7-11, 2022
and Future Prospects

Buenos Aires,
Argentina

https://indico.ictp.it/event/9840/

AGU Fall Meeting 2022

Dec. 12-16, 2022

Chicago, IL, USA

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

5th Symposium of the Committee on Space
Research (COSPAR)

Apr. 16-21, 2023

Singaporehttps://www.cospar2023.org/

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

SCOSTEP/PRESTO NewsletterVol. 33

Announcement

Location

Upcoming Meetings

Date

7

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:

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), 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.

8

SCOSTEP/PRESTO NewsletterVol. 33