SCOSTEP/PRESTONEWSLETTER
Vol. 27, April 2021

Inside this issue

Article 1:

Article 1:
1
A Spectral Solar Irradiance Monitor (SoSpIM) on
the JAXA Solar-C Space
MissionA Spectral Solar Irradiance Monitor(SoSpIM) on the JAXA Solar-C Space
Mission

Article 2:
3
A Potential Space Weather Impact on the National
Power Grid in Sudan
Article 3:
5
A New High Resolution
Solar Spectral Irradiance
Variability Model for SolarTerrestrial Studies
Highlight onYoung Scientists 1:
Juseon Bak / Korea

7

Highlight onYoung Scientists 2:
Hisashi Hayakawa / Japan

8

10

Announcement 1:
11
A New Pillar 3 Activity:
What Is the Impact ofSpectral Resolution on
Calculations of Solar Energy Deposition in the
Earth’s Atmosphere?

Announcement 2:
12News from the Office of
the SCOSTEP Scientific
Secretary

AndreaAlbertiDavid
Berghmans

Marie
Dominique

SamuelGissotHirohisa
Hara

Shinsuke
Imada

Säm
Krucker

DanielPfiffner

EugeneRozanov

Toshifumi
Shimizu

Timofei
Sukhodolov

DanielTye

Kyoko
WatanabeSilvioKollerLouise Harra, Andrea Alberti, David Berghmans, Marie Dominique, SamuelGissot, Hirohisa Hara, Shinsuke Imada, Silvio Koller, Säm Krucker, Daniel
Pfiffner, Eugene Rozanov, Toshifumi Shimizu, Timofei Sukhodolov, DanielTye, Kyoko Watanabe

Meeting Report 1:
9
The 3rd ISEE Symposium“PWING-ERG Conference
and School”
Upcoming Meetings

LouiseHarraAs a fundamental step towards answering how the plasma universe is created and evolves, and how the Sun influences the Earth and other planets in oursolar system, the JAXA Solar-C mission(Shimizu et al., 2020) is designed to comprehensively understand how mass andenergy are transferred throughout the solar

atmosphere. The EUV High-Throughput
Spectroscopic
Telescope(EUVST)
onboard does this by observing all thetemperature regimes of the atmospherefrom the chromosphere to the corona simultaneously. As well as the EUVST, there
will be a Solar Spectral Irradiance Monitor (SoSpIM). Solar-C was selected byAnnouncement 3:
13
NEW MEMBER COUNTRIES
Announcement 4:
14
UPDATE on the SCOSTEPVISITING SCHOLARS –2020 and 2021
Announcement 5:
SCOSTEP/PRESTO GRANTOPPORTUNITIES

14

Announcement 6:
15
SCOSTEP 2021 DISTINGUISHEDSERVICE
AWARD

Figure 1: First light images from the Lyman alpha telescope on Solar Orbiter EUI

SCOSTEP/PRESTO Newsletter・Vol. 27

Article

JAXA as the next M-class solar mission, and the launch
is in 2026.

S

oSpIM will work hand-in-hand scientifically with
EUVST, by providing the full Sun irradiance at subsecond time cadence combined with the spatially resolved spectroscopy from EUVST. The SoSPIM instrument will specifically address two aspects. These are:Highlight on Young Scientists●

Understand how the solar atmosphere becomes
unstable, releasing the energy that drives solar
flares – achieved through probing fast time cadence solar flare variations.

●

Measuring solar irradiance that impacts the Earth’s
thermosphere and the mesosphere, linking to spa- Figure 2: Simulated response of the tropical and subtially resolved measurements of the solar atmos- tropical NO (%) to the X9.3 solar flare of 6 Septemberyphere with EUVST.
2017.

I

Meeting Reportn order to achieve these goals, the SoSpIM instrument will monitor the spectrally resolved solar irradiance with sub-second time cadence. A key advantage of
having a ‘Sun-as-a-star’ instrument onboard the missionis that all solar flares will be visible from Earth. SoSpIM will provide high time resolution measurements
in 2 channels (a) in the corona through channel 1(EUV) and (b) in the lower atmosphere through channel
2 (Lyman alpha). Lyman-alpha is known to be the mostprominent line of the solar spectrum and is formed in
the mid- and upper-chromosphere. The recently
launched Solar Orbiter carries a Lyman alpha imager(see Figure 1), and will provide an insight to the spatial
location of Lyman alpha emission.

W

Upcoming Meetingse intend to use SoSpIM data for the now-castingof the Earth’s upper atmosphere in response to
the solar irradiance enhancement caused by solar flares(e.g. TIME-GCM, Qian et al, 2009, and a new model
GAIA, Watanabe et al., 2021, EAGLE model,Bessarab
et al., 2020) An example is shown using the EAGLE
model to study the atmospheric response to X9.3 flareon 06.09.2017 and showed pronounced response of theatmospheric state. Figure 2 illustrates simulated tropical
NOy signal (%) relative to the background. Highly significant NOy increase by up to 150% is visible in theupper mesosphere. We expect a more accurate solar
irradiance data forecast obtained from the SOLAR-C
space mission data.

Announcement
2

SCOSTEP/PRESTO Newsletter・Vol. 27

References
Bessarab F.S., Sukhodolov T.V., Klimenko M.V.,
Klimenko V.V., Korenkov Yu.N., Funke B., Zakharenkova I. E., Wissing J.M., Rozanov E.V.: Ionospheric
response to solar and magnetospheric protons during
January 15-22, 2005: EAGLE whole atmosphere model
results, Advances in Space Research, ISSN 0273-1177,
https://doi.org/10.1016/j.asr.2020.10.026, 2020.
Qian, L., et al., 'Flare location on the solar disk: Modeling the thermosphere and ionosphere response' Journalof Geophysical Reserch, Vol. 115, A09311,
doi:10.1029/2009JA015225 (2010).
Shimizu, T., et al, ‘The Solar-C (EUVST) mission: thelatest status’ Proceedings of the SPIE, Volume 11444,
id. 114440N 7 pp. (2020).

Article

Article 2:

A Potential Space Weather Impact on the National
Power Grid in Sudan

Highlight on Young Scientists

Magdi Elfadil Yousif Suliman1
1College of Science, Physics Department, Sudan University of Science and Technology(SUST), Khartoum, Sudan; magdielfadil@gmail.com.

Magdi Elfadil
Yousif Suliman

I

Meeting Reportn magnetosphere electrodynamics, several disturbances coupled to earth electromagnetic structure havebeen known to elucidate the impact on several conducting metallic based long systems. For instance, impact on
power grids could be inducing currents that penetrate
into them, known as geomagnetically induced currents(GICs). However, observations records of this impact
dominate systems that located in/close to higher latitudes, where disturbance driven amplitudes electrojets
are localized. Nevertheless, observations of such ground
impact at low- mid latitudes have been attributed to other mechanisms, rather than the disturbances amplitudeenhancements, i.e. to disturbances spectral content.
However, there have been numerous of studies that reported evidencing of GICs enhancements in low-mid
latitude locations, see e.g.[1][2][3][4][5].

I

T(MAGDAS) of Kyushu University, Japan[8]; further
investigations were carried out on these 18 blackouts
events in order to proof spectral content, by checking
dynamic magnetograms for the occurrence of continues
pulsations. Results showed occurrence of low –mid latitude Pc5 pulsations globally distributed, mostly global
mode, see Figure 2.

Announcement

his study focuses on to carry out investigations on
the possibility of space weather disturbances spectral content to cause blackouts in the power grid in Sudan. The date and time of blackouts records, in the power grid in the period 2001-2013, were collected from theSudanese Electricity Distribution Company Ltd(SEDC), Soba Center[6]. Preliminary investigations
were carried out by checking the corresponding timeseries plots of the final Dst index data[7], for the occurrence of features of storms, storm sudden commencement (SC) type of storms, and sudden impulse (SI)within date and time of blackouts. Results of these preliminary investigations were so interesting that 18 out of
total 37 blackouts events records were correspond to a
Dst showing variety features, e.g. recovery phase of asevere SC storm (DST≤ -150nT), initial, main and recovery phase of major SC storm (-50nT≥DST>-150nT),
and recovery phase of minor SC storm DST>-50nT, see
Figure 1. Moreover, using available ground geomagnetic data, obtained from some low- mid latitude observatories of the chain of Magnetic Data Acquisition System

Figure1 : Upper part is a pie chart showing blackout
events records during the time span: 2001: 2013, itshows 49 % of blackout events happened within variety
features shown by the final Dst index[7], e.g. 14% (redcolor part in the pie chart) of blackout events happened
within a recovery phase of major storms, a sudden commencement (SC) type of storms; While the lower partshows occurrence of blackouts Vs years in the timespan: 2001: 2013, the arrows indicate dates when blackout events recorded, in Day/Month format.

Upcoming Meetingsmportantly, investigations of hazardous GIC impact
on power grids in low- mid latitude locations becomeof great interest, in particular most of these locations lay
where developing or least developed countries are located. Power grids in such countries are more vulnerable tooutages and maintenance challenges. Consequently,
economics and societal effects of space weather impact
on power grids in these countries are much serious.

To this end, it is very important to urge maintenanceof the single and the only geomagnetic ground observatory in Sudan, which belongs to the MAGDAS
chain of observatories. Additionally, it is also necessary
to stimulate accomplishment of future campaigns to
deploy observatories in the country, not just limited tomagnetometers but could include ionospheric probes.
We undertake responsibility to continue future network-

SCOSTEP/PRESTO Newsletter・Vol. 27

3Article

ing in order to attract international scientific community
concern for supporting us to reach our ultimate goal
which is to be able to locally model GIC in Sudan.
References

Highlight on Young Scientists[1] Kappenman JG. Storm sudden commencement
events and the associated geomagnetically induced current risks to ground-based systems at low-latitude andmidlatitude locations. Space Weather. 2003;1(3).
[2] Watari S, Kunitake M, Kitamura K, Hori T, Kikuchi
T, Shiokawa K, Nishitani N, Kataoka R, Kamide Y, Aso
T, et al. Measurements of geomagnetically induced current in a power grid in Hokaido, Japan. Space Weather.
2009;7.
[3] Ngwira CM, McKinnell LA, Cilliers PJ. Geomagnetic activity indicators for geomagnetically induced current
studies in South Africa. Advances in Space Research.
2011;48:529-534.
[4] Zhang JJ, Wang C, Sun TR, Liu CM, Wang KR. GIC
due to storm sudden commencement in low-latitude high-voltage power network in China: Observation and simulation. Space Weather. 2015;13:643-655.

Meeting Report[5] Kai-rang W, Lian-guang L, Yan L. Preliminary analysis on the interplanetary cause of geomagnetically induced current and its effect on power systems. Chinese
Astronomy and Astrophysics. 2015;39:78-88.
[6] Sudanese Electricity Distribution Company Ltd(SEDC). [Internet]. 2015 [cited 2021 Feb 26]. Available
from: https://www.sedc.com.sd/control.
[7] Nose M, Sugiura M, Kamei T, Iyemori T, Koyama Y.
World Data Center. [Internet]. 2015 [cited 2021 Feb 26].
Available from: http://wdc.kugi.kyoto-u.ac.jp/dst_final/
index.html.

Upcoming Meetings[8] Yumoto K, and MAGDAS Group. Space weather
activities at SERC for IHY: MAGDAS. Bulletin of the
Astronomical Society of India. 2007;35:511-522.

Announcement
4

Figure 2: show stacked magnetograms of three low- midlatitude ground magnetometers stations of the MAGDAS[8] chain, from upper to lower: Camden (CMD) ( L-value is 1.94), Hermanus (HER) (L-value is 1.83), andSanta Maria (SMA) (L-value is 1.12), respectively; between the rectangle shape it shows a simultaneous global
pulsations continuous (Pc) pulsations (filtered frequencies range are: 1:10 mHz), with global distribution appearance, mainly a Pc 5 (range: 1.67: 6.67 mHz), these
pulsations are within the time of the blackout event of
the day: January 12, 2008.

SCOSTEP/PRESTO Newsletter・Vol. 27

Article

Article 3:

A New High Resolution Solar Spectral Irradiance
Variability Model for Solar-Terrestrial
Studies

Highlight on Young Scientists

O. Coddington and J. Lean

Odele
CoddingtonA●

Sun-climate studies, by better capturing variability
in solar spectral features co-located with spectralfeatures in Earth atmospheric gas absorption cross Figure 1: (top) The solar irradiance spectrum at 0.1 tosections (Figure 1), and
0.3 nm spectral resolution as observed by SORCE SOL-●

solar irradiance research by better isolating varia- dependent absorption coefficients of oxygen (O 2) andble solar emission and absorption features attribut- ozone (O3) between 115 and 300 nm.
able to the Sun’s atmospheric composition, which
theoretical solar irradiance models (one example
being Shapiro et al., 2015) must accurately specify
to reliably estimate solar irradiance change (Figure
2).

Meeting Report

new solar spectral irradiance (SSI) variability
model spanning wavelengths from 115 nm to 500
nm and the time period from 1978 to 2020 has beendeveloped [Lean et al., in prep] with higher spectral
resolution than the 1-nm NRLSSI2 model that prescribes the NOAA Solar Irradiance Climate Data Record (CDR) [Coddington et al., 2016]. This new Naval
Research Laboratory model, NRLSSI2h, has spectral
resolution 0.1 nm to 310 nm and up to 0.5 nm above
that. The absolute scale and variability of the
NRLSSI2h model, when binned to 1-nm, is equivalent
to that of the NRLSSI2 model which can therefore beused to extend the new model to wavelengths beyond
500 nm. NRLSSI2h, with 10x better spectral resolution
at ultraviolet wavelengths, promises enhanced utility
for:Upcoming Meetings

STICE and AURA OMI and (bottom) the wavelength-N

Announcement

RLSSI2h and NRLSSI2 are observation-based,
empirical models, developed from space-based
SSI observations and proxies of faculae and sunspots.
The models use multiple linear regression to determine
the net incremental change in SSI that occurs withchanges in faculae and sunspots, which respectively
enhance and deplete the irradiance relative to the“quiet” irradiance level when the Sun is devoid of thesefeatures. Their proxy inputs are identical, namely the
Mg II index for facular brightening and, for sunspot
darkening, the number, area, and location of individual
sunspots. The models differ, however, in the resolutionof the space-based SSI observations used to formulate
the model coefficients. For NRLSSI2, these were Solar

Figure 2: The ultraviolet and visible spectrum of irradiance change over the 11-year solar cycle estimated by theempirical NRLSSI2 and NRLSSI2h models and a theoretical solar radiative transfer code. The higher spectral
resolution of the NRLSSI2h model better isolates theenhanced variability in solar lines.

Radiation and Climate Experiment (SORCE) observations spanning 115 nm to 2400 nm and binned to 1-nm.

SCOSTEP/PRESTO Newsletter・Vol. 27

5Article
Highlight on Young Scientists

For NRLSSI2h, SORCE observations from 115 nm to
310 nm at their native 0.1 nm resolution were combinedwith AURA Ozone Monitoring Instrument (OMI) observations from 310 nm to 500 nm at 0.3 nm to 0.5 nm resolution. NRLSSI2 model validation with independent
SSI observations demonstrated its superior performance
relative to alternative solar irradiance variability models
at wavelengths up to 500 nm on time periods of several
solar rotation cycles [Coddington et al., 2019]. As solar
cycle 25 activity continues to increase, additional model
validation is made possible by the high-quality observations of the TSIS-1 mission (Figure 3) that is continuing
the daily space-based solar irradiance record into thepost-SORCE era [Coddington and Woods, 2020]. The
TSIS observations also provide the absolute scale for a
new SSI reference spectrum of at least 0.01 spectral resolution spanning 202 to 2730 nm [Coddington et al.,2021]; several variants are also produced at lower, fixed,
spectral resolution. Recently, this new reference spectrum has been extended from 115 to 200,000 nm[Coddington et al., in prep].

Figure 4: The solar cycle change in the vertical profile ofEarth atmospheric energy deposition in the Lymanalpha band (121-122 nm) when using the NRLSSI2 and
NRLSSI2h models as the solar forcing input.

References

Meeting Report

Coddington, O., J. Lean, P. Pilewskie, M. Snow, and D.
Lindholm (2016), A solar irradiance climate data record,
Bull. Amer. Meteor. Soc., doi:10.1175/BAMS-D-1400265.1.

Upcoming Meetings
Announcement
6

Coddington, O., J. Lean, P. Pilewskie, M. Snow, E. Richard, G. Kopp, S. Béland, C. Lindholm, M. DeLand, S.
Marchenko, M. Haberreiter, and T. Baranyi (2019), Solar
Irradiance Variability: Comparisons of Models andMeasurements, Earth and Space Science, special issue:
Results from the Initial Solar Irradiance Science Team
(SIST)
program,
6,2525-2555.
https://
doi.org/10.1029/2019EA000693.
Coddington, O., E. C. Richard, D. Harber, P. Pilewskie,
T. N. Woods, K. V. Chance, X. Liu, and K. Sun (2021),
The TSIS-1 Hybrid Solar Reference Spectrum, Earth andSpace Science Open Archive, doi: 10.1002/
essoar.10506142.1 (under consideration at Geophys.
Res. Lett.)
Figure 3: The ultraviolet and visible spectrum of irradiance change during a sunspot-dominated solar rotationin late November, 2020 as observed by the TSIS-1 SIM
instrument at variable resolution and modeled by
NRLSSI2 and NRLSSI2h.

Coddington, O., and T. N. Woods (2020), An Overview
of the Total and Spectral Solar Irradiance Sensor (TSIS1) Mission, SCOSTEP/PRESTO Newsletter, Vol., 24,
July 2020.

T

Lean, J., O. Coddington, S. V. Marchenko, M. T.
DeLand, and M. Snow (2021), A New Model of Solar
Ultraviolet Irradiance Variability with 0.1-0.5 nm Spectral Resolution, in preparation.

hese new high-resolution datasets - the daily
NRLSSI2h estimates and the absolute irradiancereference spectrum – add value to the various solar irradiance and Sun-climate research activities performed by
SCOSTEP members. For example, initial estimates suggest the peak oxygen absorption of solar HI Lyman alpha radiation shifts to lower altitudes when estimatedusing NRLSSI2h instead of NRLSSI2 (Figure 4).

SCOSTEP/PRESTO Newsletter・Vol. 27

Shapiro, A. I., S. K. Solanki, N. A. Krivova, R. V. Tagirov, and W. K. Schmutz (2015), The role of the Fraunhofer lines in solar brightness variability, A&A, 581, A116.
https://doi.org/10.1051/0004-6361/201526483.

Article

Highlight on Young Scientists 1:

Verification of Solar Spectral Irradiance on Exploiting Trace-Gas Concentrations from Satellite
Measurements

O

JuseonBakommend the use of the TSIS-1 HSRS for trace-gas retrievals from UV measurements.

Meeting Reportzone Monitoring Instrument (OMI) has been remotely sensing ozone layer and key air pollutants(O3, NO2, and aerosols) from space since 2004. It
measures backscattered radiation in 270-500 nm, alongwith measurements of the solar irradiance. The retrievalof ozone profiles from the spectral range 270-330 nm is
highly sensitive to wavelength and slit function uncertainties and forward model simulation errors. A well calibrated high-resolution solar spectral irradiance is of importance for characterizing wavelength assignment andslit functions by means of matching the solar Fraunhofer
absorption lines between measured and reference spectra
as well as for convolution process in forward model simulation.

Highlight on Young Scientists

Juseon Bak
Institute of Environmental Studies, Pusan National University, Busan, Korea

I

Figure 2. (a) Impacts of using different solar reference
datasets on fitting slit widths from OMI irradiancemeasurements. Note that slit widths represent a Fullwidth at Half Maximum (FWHM) of Gaussian slit function.
Residuals
arecalculated
as
where

Upcoming Meetingsn this work we focused on impacts on OMI ozone profiles retrievals due to switching the current solar reference (SAO20101) to the recently published solar reference (TSIS-1 HSRS2) which spans 202 nm to 2730 nm at
0.01 to ~ 0.001 nm spectral resolution. As shown in
Fig.1, radiometric uncertainties of SAO2010 range from
10-25 % below ~ 305 nm to ±5% above, but TSIS-1
HSRS are excellently matched with the reference within~ 1 % or less over the spectral range. In fitting OMI slit
shapes as a Gaussian, derived slit widths differ by 0.02
nm due to different solar reference datasets, with fitting
uncertainties being smaller (by 0.5 %) when TSIS-1
HSRS is used as a reference to OMI irradiance measurements. In performing ozone retrievals from OMI earthshine measurements, the fitting residuals decrease by up
to ~ 5 % due to using the new solar reference data while
relative changes of ~ 2-3 % in tropospheric column
ozone (Fig.2). Based on this study, we would like to rec-is measured/simulated spectrum. (b) Same as (a), but for performingozone retrievals from OMI radiance measurements; In
left panels, the evaluated variables are derived whenusing TSIS-1 HSRS, with comparison to SAO2010 based
retrievals in right panels (SAO2010 – TSIS-1 HSRS).

Data Availably
1

SAO2010:https://www.cfa.harvard.edu/atmosphere/
links/sao2010.solref.converted

Announcement

2

TSIS-1 HSRS: https://www.essoar.org/doi/10.1002/
essoar.10506142.1
Acknowledgement
This work is funded by Basic Science Research Program
through the National Research Foundation of Korea
Figure 1: Evaluation of irradiance scales of high- (NRF) funded by the Ministry of Education
resolution solar reference datasets against TSIS-1 (2020R1A6A1A03044834).
SIM reference spectrum at spectral resolution of
TSIS-1 SIM, with the mean values of individual differences below and above 305 nm.

SCOSTEP/PRESTO Newsletter・Vol. 27

7Highlight on Young Scientists 2:

ArticleAnalyses of Historical Extreme Space Weather
EventsHighlight on Young Scientists

Hisashi Hayakawa
Institute for Space-Earth Environmental Research and Institute for Advanced Research,
Nagoya University, Japan

HisashiHayakawa

analyses of extreme geomagnetic storms One superstorm (in October 1903; minimum Dst* ≈ Q uantitative
are beyond just scientific interests. Our ever- 531 nT; Figure 2) even occurred immediately after theincreasing dependency on technological infrastructure
has made our society increasingly vulnerable to thesestorms (Riley et al., 2018). Nevertheless, their occurrences are significantly rare. Although the standard Dst
index has been used since the International GeophysicalYear (IGY: 1957–1958), only five geomagnetic storms
surpassed the extreme‑storm threshold (minimum Dst ≤-400 nT) during this interval, and only one was identified as a superstorm (minimum Dst ≤ -500 nT) (Riley etal., 2018; Meng et al., 2019).

minimum of a weak solar cycle (Hayakawa et al.,2020a). This and similar case studies will form the basis
for future discussions on extreme geomagnetic storms.

Meeting ReportC

ontrastingly, historical evidence shows that there
were more extreme storms and superstorms before
the IGY. The geomagnetic superstorms of September
1859, February 1872, and May 1921 have been considered as benchmarks (minimum Dst ≈ -900 nT) of suchextreme weather events (Cliver and Dietrich, 2013;
Hayakawa et al., 2018, 2019b). In this case report, ourteam has reconstructed the Dst estimates (Dst*) withdata completeness and reasonable longitudinal separations for historical storms using historical magnetograms in the mid/low magnetic latitude.
2: Dst* time series for the geomagnetic superur team has identified at least four geomagnetic Figurestorm in October 1903 (Hayakawa et al., 2020a).
superstorms between 1900 and 1956 based on theabovementioned benchmarks; accordingly, we have re- Acknowledgment
constructed the Dst* time series of these four superstorms and measured their magnitudes (Figure 1). With This work was supported in part by JSPS Grant-in-Aids
respect to the most powerful geomagnetic storm by the JP17J06954 and JP20K22367, JSPS Overseas Chalstandard Dst index (the March 1989 storm; minimum lenge Program for Young Researchers, the 2020 YLC
Dst = -589 nT; Boteler, 2019), these results have quanti- collaborating research fund, and the research grants fortatively visualised unique cases of historical geomagnet- Mission Research on Sustainable Humanosphere fromic superstorms surpassing this benchmark (Hayakawa et Research Institute for Sustainable Humanosphereal., 2019a, 2020a, 2020b; Love et al., 2019a, 2019b). (RISH) of Kyoto University and Young Leader Cultivation (YLC) program of Nagoya University. Our teamthanks WDC for Geomagnetism at Edinburgh forproviding geomagnetic baselines and British magnetograms, WDC for Geomagnetism at Kyoto for providing
the Dst index and individual magnetic measurements,and WDC SILSO for providing international sunspot
numbers.

O
Upcoming Meetings
Announcement

References
Boteler, D. H.: 2019, Space Weather, 17, 1427–1441.
Clette, F., Lefèvre, L.: 2016, Solar Physics, 291, 2629–
2651.
Cliver, E. W., Dietrich, W. F.: 2013, Journal of Space
Weather and Space Climate, 3, A31.
Figure 1: Geomagnetic superstorms contextualised upon Hayakawa, H., et al.: 2018, The Astrophysical Journal,
the solar cycles based on the SILSO International Sun- 862, 15.
spot Number (Clette and Lefèvre, 2016).

8

SCOSTEP/PRESTO Newsletter・Vol. 27

Love, J. J., Hayakawa, H., Cliver, E. W.: 2019a, Space
Weather, 17, 37-45.
Love, J. J., Hayakawa, H., Cliver, E. W.: 2019b, Space
Weather, 17, 1281–1292.
Meng, X., et al.: 2019, Journal of Geophysical Research:
Space Physics, 124, 3926–3948,
Riley, P., et al.: 2018, Space Science Reviews, 214, 21.

ArticleHayakawa, H., et al.: 2019b, Space Weather, 17, 15531569.
Hayakawa, H., et al.: 2019a, Monthly Notices of theRoyal Astronomical Society, 484, 4083-4099.
Hayakawa, H., et al.: 2020a, The A strophysical Journal
Letters, 897, L10.
Hayakawa, H., et al.: 2020b, Monthly Notices of theRoyal Astronomical Society, 497, 5507-5517.

Highlight on Young Scientists

Meeting Report 1:

The 3rd ISEE Symposium “PWING-ERG Conference
and School”
Kazuo Shiokawa1, Yoshizumi Miyoshi1, and Iku Shinohara2
1Institute for Space-Earth Environmental Research (ISEE), Nagoya University, Japan
2Institute of Space and Astronautical Science (ISAS), Japan
Aerospace Exploration Agency (JAXA), Japan

Yoshizumi
Miyoshi

Iku
Shinoharatries have registered in this conference and joined discussion on the dynamics of the inner magnetosphere basedon latest ground and satellite measurements and modeling. This conference was supported by ISEE, Nagoya
University, JSPS (PWING project: 16H06286), ISAS/JAXA (Arase Project), NICT, SCOSTEP, and SGEPSS.
The conference site with details of the conference andschool is at https://is.isee.nagoya-u.ac.jp/pwing-erg/.

Meeting ReportT

he 3rd ISEE Symposium “PWING-ERG Conference
and School” was held on March 8-12, 2021 via
online. This conference was held as the completion of
the PWING project and as the 5th year anniversary of
the ERG (Arase) mission. The school was held in thefirst 1.5 days with six lectures and two training courses
for graduate-course students. The ISEE Award presentation and commemorative lecture was held in the afternoon of March 11. The 264 participants from 37 coun-

Kazuo
Shiokawa

Upcoming Meetings
Announcement

Figure 1: Zoom Group Photo of the participants of the PWING-ERG Conference and School (multiple pages are
combined with some overlaps)

SCOSTEP/PRESTO Newsletter・Vol. 27

9Article

Upcoming meetings related to SCOSTEPHighlight on Young Scientists

Conference

Date

LocationContact Information

EGU General Assembly 2021

Apr. 25-30, 2021

Vienna, Austria

https://www.egu2021.eu/

ISWI/SCOSTEP Iberian Space Science Summer School

July 26-30, 2021

OnlineMeeting Report
Upcoming Meetings

AOGS 2021

Aug. 1-6, 2021

Suntec, Singapore

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

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

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://scostep.org/stp-symposia/

EGU General Assembly 2022

Apr. 3-8, 2022

Vienna, Austria

COSPAR 2022

Jul. 16-24, 2022

Athens, Greece

AOGS 2022

Aug. 14-19, 2022

Melbourne, Australia

AGU Fall Meeting 2022

Dec. 12-16, 2022

Chicago, IL, USA

IUGG 2023

In July, 2023

Berlin, Germany

AGU Fall Meeting 2023

Dec. 11-15, 2023

San Francisco, CA,USA

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

Announcement
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SCOSTEP/PRESTO Newsletter・Vol. 27

http://
www.cosparathens2022.org/

https://www.agu.org/fall-meetinghttps://www.agu.org/fall-meetingArticleAnnouncement 1:

A New Pillar 3 Activity: What Is the Impact of Spectral Resolution on Calculations of Solar Energy
Deposition in the Earth’s Atmosphere?

Highlight on Young Scientists

O. Coddington and S. Misios
Odele
Coddington

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to 500 nm relative to that of the current, operational, 1nm resolution NRLSSI2 model that spans a broader
wavelength range and longer time period.

These new solar irradiance datasets provide an opportunity to update the default SSI used to model themean state of the atmosphere and to evaluate Earth’s
response to solar forcing at higher spectral resolution.
Molecules in Earth’s atmosphere, such as oxygen andozone, alter the incoming solar irradiance through wavelength-dependent absorption and photochemical effects,
which in turn affects atmosphere temperatures and drives
dynamical variability, particularly at heights greater 50
km. For example, one initial estimate suggests the peakoxygen absorption of solar HI Lyman a radiation shifts
to lower altitudes when estimated using NRLSSI2h as
opposed to NRLSSI2 [Coddington and Lean, 2021]. A

Meeting Report

ew datasets of solar spectral irradiance (SSI) at
higher spectral resolution have recently been developed. For example, the TSIS-1 SSI observations withdifferences approaching 10% at some wavelengths fromother reported solar irradiance spectra [Coddington andWoods, 2020], forms the basis of a new solar irradiancereference spectrum spanning 202 to 2730 nm with aspectral resolution of at least 0.01 nm developed by adjusting high spectral resolution solar line data to the irradiance scale of the more accurate, but lower spectral resolution, TSIS-1 Spectral Irradiance Monitor (SIM) instrument [Coddington et al., 2021]. Additionally, a new
Naval Research Laboratory (NRL) solar irradiance variability model, called NRLSSI2h, was recently developed[Lean et al., in prep; Coddington and Lean, 2021]. It
spans the years 1978 through 2020 and has up to 10x
greater spectral resolution at wavelengths from 115 nm

Stergios
MisiosUpcoming Meetings
Announcement

Figure 1: Differences in the resolution of the extraterrestrial solar spectral irradiance (left) impact the depth of theatmospheric deposition within Earth’s atmosphere as estimated with the Modtran 6.0 radiative transfer software
package (right).

SCOSTEP/PRESTO Newsletter・Vol. 27

11Article
Highlight on Young Scientists
Meeting Report
Upcoming Meetings
Announcement
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second initial estimate suggests changes also occur in thedeposition depths of solar irradiance at longer wavelengths (Figure 1).

Chemistry-climate models play an important role inidentifying the response of Earth’s atmosphere tochanges in the absolute magnitude and variability of thesolar forcing because they contain a myriad of the radiative and chemical processes that simulate Earth’s climate. Would these models extract new information about
Earth’s climate when considering higher spectral resolution solar features potentially co-located with spectralfeatures of absorbing gases in Earth’s atmosphere? To
address
thisquestion,
Odele
Coddington(odele.coddington@lasp.colorado.edu) and Stergios Misios (smisios@noa.gr) are seeking to develop a working
group under PRESTO Pillar 3 to apply these new solar
irradiance datasets in comparative chemistry-climate
model studies of the impact of spectral resolution on
calculations of solar energy deposition in the Earth’s
atmosphere. We invite SCOSTEP members to initiate
their interest in this activity through an initial email. Thisemail list will be used to form the basis of the new working group to guide the scope and architecture for the targeted climate modeling studies.

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ance variability estimates are available for use by the
SCOSTEP community for these studies.

References
Coddington, O., and T. N. Woods (2020), An Overview
of the Total and Spectral Solar Irradiance Sensor (TSIS1) Mission, SCOSTEP/PRESTO Newsletter, Vol. 24,
July 2020.
Coddington, O., and J. Lean (2021), A New High Resolution Solar Spectral Irradiance Variability Model for
Solar-Terrestrial Studies, SCOSTEP/PRESTO Newsletter, Vol. 27, April 2021.
Coddington, O., E. C. Richard, D. Harber, P. Pilewskie,
T. N. Woods, K. V. Chance, X. Liu, and K. Sun (2021),
The TSIS-1 Hybrid Solar Reference Spectrum, Earth andSpace Science Open Archive, doi: 10.1002/
essoar.10506142.1 (under consideration at Geophys.
Res. Lett.)
Lean et al., O. Coddington, S. V. Marchenko, M. T.
DeLand, and M. Snow (2021), A New Model of Solar
Ultraviolet Irradiance Variability with 0.1-0.5 nm Spectral resolution (in prep).

iles of the TSIS-1 daily irradiance, the hybrid absolute reference spectrum and the NRLSSI2h irradi-

Announcement 2:

News from the Office of the SCOSTEP Scientific
Secretary
Patricia Doherty
SCOSTEP Scientific Secretary, Institute for Scientific Research (ISR), Boston College, Boston,
MA, USA

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he office of the SCOSTEP Scientific Secretary has
been active with a new membership drive, the Visiting Scholar Program, grant funding opportunities and the2021 Distinguished Service Award.
e have also recently activated a dedicated website
to SCOSTEP and a twitter account. Please view
the website at: https://scostep.org. The website will be
updated regularly for new opportunities and information
relevant to our membership.
Please also follow
SCOSTEP on Twitter: @scostep1 and encourage the useof #scostep in your own solar-terrestrial tweets.

SCOSTEP/PRESTO Newsletter・Vol. 27

Patricia
Dohertyf you are not already enrolled in our mailing list,
please send a note to scostep[at]bc.edu to be added tothis mailing list. All announcements and updates arebroadcast to the mailing list.
inally, if you have any questions related to the activities and opportunities of SCOSTEP, please contact
me the Office of the SCOSTEP Scientific Secretary at
scostep[at]bc.edu.

ArticleAnnouncement 3:

NEW MEMBER COUNTRIESHighlight on Young Scientists

Patricia Doherty
SCOSTEP Scientific Secretary, Institute for Scientific Research (ISR), Boston College, Boston, MA, USAWPe are pleased to announce that Poland has joined
SCOSTEP as a member country.

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COSTEP has three main activities that address theneeds of the solar terrestrial physics community
worldwide: (1) Scientific programs, (2) Capacity building and outreach, (3) International Scientific Meetings.
A SCOSTEP member country will have a say in the policy and functioning of SCOSTEP because the country
will be represented in the SCOSTEP Council by a National Adherent Representative. The National Adherent

ountries are now invited to apply for membership.
The process begins with a responsible scientificbody writing to the President of SCOSTEP seeking
membership. The application letter should include thefollowing: (i) list of solar-terrestrial physics activities in
the country and the institutions that carry out these activities, (ii) the name and address of the responsible institution, (iii) the membership category, and (iv) the proposed name of the National Adherent Representative.
After approval by the Bureau, the application will bepresented to the SCOSTEP Council, which considers
and acts on the admission of new member nations.
In most countries the Academy of Sciences administers
SCOSTEP affairs including selecting the National Adherent Representative from the solar-terrestrial physics
community to the SCOSTEP General Council (GC) andsending annual dues to the SCOSTEP secretariat.

Upcoming Meetings

COSTEP is actively seeking new member countries. A member ship committee, chaired by Dr.
Jorge Chau of the Leibniz-Institute of AtmosphericPhysics, is actively identifying and reaching out to potential member countries. Please contact Jorge Chau or
Patricia Doherty for more information.

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Meeting Reportoland is sponsored by the Space Research Centre of the Polish Academy of Science in Warsaw.
Institutions active in solar-terrestrial physics in Poland
include the Space Research Centre, the Institute of Geophysics and the Institute of Geological Sciences of thePolish Academy of Science. In addition programs areactive at a number of universities including the University of Warsaw, the University of Warmia and Mazury,
Wroclaw University, the University of Zielona Gora andthe Military University of Technology. The National
Adherent Representative for Poland is Dr. Hanna Rothkaehl, Head of the Space Plasma Physics Department at
the Space Research Center, Polish Academy of Science.

Representative serves as a close liaison between
SCOSTEP and the respective Adherents. The National
Adherent Representatives also provide valuable advicein establishing the SCOSTEP scientific programs and as
members of the General Council (GC) the Adherents
participate in the governing and decision making of
SCOSTEP.

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or more information on country membership applications, please contact the Scientific Secretary(SCOSTEP [at] bc.edu).

Announcement

SCOSTEP/PRESTO Newsletter・Vol. 27

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Announcement 4:

ArticleUPDATE on the SCOSTEP VISITING SCHOLARS –2020 and 2021

Highlight on Young Scientists

Patricia Doherty
SCOSTEP Scientific Secretary, Institute for Scientific Research (ISR), Boston College, Boston, MA, USAT

he purpose of the SCOSTEP Visiting Scholar (SVS)
Program is to provide training for graduate students
from developing countries in established laboratories ofsolar-terrestrial physics for periods of 1 to 3 months.

Due to the travel restrictions imposed by the COVID
pandemic, most of the SVS 2020 awardees have notyet started their training programs. As such, the 2020
recipients of the SCOSTEP SVS program have until theend of 2021 to complete their training program, with the

Meeting Report
Upcoming Meetings
Announcement14agreement of the host laboratory.

An announcement for the 2021 SVS applications wasmade on January 15, 2021 with a deadline of February 28, 2021. The awardees of the 2021 program will beannounced soon. The 2021 SVS recipients will have until the end of 2022 to complete their training period.

For more information on the SVS program, please
visit the SCOSTEP website: https://scostep.org/svs

Announcement 5:

SCOSTEP/PRESTO GRANT OPPORTUNITIESPatricia Doherty
SCOSTEP Scientific Secretary, Institute for Scientific Research (ISR), Boston College, Boston, MA, USAS

COSTEP/PRESTO has funding opportunities available to support campaigns, meetings and databases
relevant to the PRESTO themes.

Campaigns and Meetings: ProS COSTEP/PRESTO
posals are accepted annually to support campaigns

and meetings relative to the PRESTO topics. The deadline for proposals for 2021 was December 31, 2020. The
Scientific Secretary is currently working with the 2021
awardees to support these awards. More information onthese activities will be provided in reports from theawardees following the activities. Announcements ofopportunity will be issued in September 2021 for the2022 award period.

Databases: A new AnnounceS COSTEP/PRESTO
ment of Opportunity was recently released for

SCOSTEP/PRESTO Database Proposals.
These
grants are to support the development of databases ofsolar-terrestrial data that are strictly related to one ormore PRESTO Pillars and contribute to the PRESTOSCOSTEP/PRESTO Newsletter・Vol. 27

activities. PRESTO funding for databases will be up to$5000 USD. The grants can be used to cover expenses
for software, manpower, computer servers, web-site
maintenance. The deadline for the proposals is April 1,
2021. More information is available on the database proposals is on the SCOSTEP website: https://scostep.org/
grant-proposals/
Capacity Building Funds: SCOSTEP is
S COSTEP
currently accepting proposals for organizing schools

for capacity building of students and young scientists insolar-terrestrial physics by (1) providing up to $5000 forparticipant support and by (2) endorsing lecturers for theschool from SCOSTEP Science Disciplinary Representatives (SDRs), National Adherent Representatives andother SCOSTEP-related officers.
Please see the
SCOSTEP website for more information: https://
scostep.org/capacity-building/Announcement 6:

ArticleSCOSTEP 2021 DISTINGUISHED SERVICE AWARDSCOSTEP is pleased to announce that the2021 Distinguished Service Award is given toHighlight on Young Scientists

Dr. Franz-Josef Lübken
Director, Leibniz Institute for Atmospheric Physics (IAP)
Professor, University of Rostock, Germany

Franz-Josef
LübkenCitation: For unique and meritorious service to SCOSTEP activities and interests at an international level,
which have visibly influenced outreach and high-level research in solar-terrestrial physics.

DW
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o further the success of CAWSES, Dr. Lübken
chaired the team to define the program for CAWSES-II for 2009-2013. A certainly outstanding successwithin CAWSES-II was the organization of the
SCOSTEP Symposium STP-12 in Berlin in 2010. The
exciting program and opportunities to build strong networks is a hallmark success of CAWSES II. During thistime, he further engaged the CAWSES community inDuring VarSITI (2014-2018), Dr. Lübken led the scientific element ROSMIC which included four
working groups from solar influences to vertical atmosphere coupling. Within ROSMIC, several modelling andinstrumental campaigns were proposed and realized.

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ducation and capacity building within SCOSTEP
were further essential interests of Dr. Lübken. As the
Director of IAP, he committed IAP to engage with the
SCOSTEP Visiting Scholar Program. He also gave lectures at the 2013 ISWI/SCOSTEP School on Space Sciences held in Nairobi, Kenya. Besides his many international efforts Dr. Lübken’s engagement to expand anddevelop SCOSTEP topics within Germany has been outstanding.

Upcoming Meetings

ithin CAWSES (2004-2008), Dr. Lübken waschair of the Scientific Theme “Atmospheric Coupling Processes” that included three working groups andinitiated eight projects dedicated to hydro- and electrodynamic processes from the polar to equatorial middle atmosphere and ionosphere.

compiling special topical sections in international ISIlisted journals such as JGR, thereby ensuring the international visibility of new results from SCOSTEP.

Meeting Reportr. Franz-Josef Lübken is recognized as a dedicatedscientific member of various SCOSTEP entities
and has contributed to make SCOSTEP a lively international network resulting in original research and outstanding education. His dedication is demonstrated byhis commitment to serve as Vice-President of SCOSTEP
from 2011-2019 and his outstanding contributions to thescientific programs of SCOSTEP. He has also served as
the Chairman of the German SCOSTEP Committee since
2010.

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his award recognizes Dr. Lübken’s many unique andmeritorious services to SCOSTEP activities andinterests at an international level, which have visibly influenced outreach and high-level research in solarterrestrial physics.

Announcement

SCOSTEP/PRESTO Newsletter・Vol. 27

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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

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SCOSTEP/PRESTO Newsletter・Vol. 27