SCOSTEP/PRESTONEWSLETTER
Vol. 29, October 2021

Inside this issue

Article 1:

Article 1:1
New 14C-Based Reconstructions of 11-Year
Solar Cycles: Longer
Than a Millennium Now

New 14C-Based Reconstructions of
11-Year Solar Cycles: Longer
Than a Millennium Now

Article 2:
3
Diagnosing AtmosphericPlanetary-Scale
Waves Through MultiStation Approaches
Highlight onYoung Scientists 1:
Ange Cynthia Umuhire/ Rwanda

Ilya G.
Usoskin6

Highlight on
8Young Scientists 2:
Theodosios Chatzistergos / Germany
10
Meeting Report 1:The
1st
SummerSchool on Space Research, Technology &Applications for Young
Scientists and PhD Students
Meeting Report 2:
11
i4s – First IberianSpace Science Summer
SchoolUpcoming Meetings

Ilya G. Usoskin1
1University of Oulu, FinlandIt was known for a long time that dark
spots, occasionally observable by naked
eyes, can appear on the Sun, but their nature and even very belonging to the Sun
was unclear. Scientifically, the sunspots
were discovered and confirmed as such in
the earlier 17th century (see a review by
Arlt & Vaquero, 2020). The main patternof sunspots occurrence is that they tend to
appear in the course of the solar cycle
which takes about 11 years on average(Hathaway, 2015). The existence of the 11-year cycle was first proposed by the Danish astronomer Christian Horrebow in the
18th century and finally discovered by theGerman astronomer Samuel Heinrich
Schwabe in the middle 19th century. It is
now called the Schwabe cycle with a du-ration of about 11 years on average ranging from 8 to 16 years for individual cycles. Solar cycles are subsequently numbered by Rudolf Wolf starting from 1749.
The period covered by telescopic sunspot
observations since 1610, includes also theMaunder minimum, viz. the period ofvery low solar activity when the Sun displayed virtually no spots (Eddy, 1976).

For the period before 1610, solar variability can only be studied using indirect cosmogenic-isotope proxy datasets(Beer et al., 2012; Usoskin, 2017), which
are usually of low temporal resolution andcannot resolve individual solar cycles. A
breakthrough has been made recently
thanks to the high-precision annual meas-

12

Announcement1:
13
VarSITI Review Papers
Are Published in theOpen Access PEPS
JournalFigure 1. Sunspot numbers reconstructed from annual Δ14C data (black line) with
±1σ uncertainties (grey shading) for the period 971—1900 (digital data are available
in Usoskin et al., 2021). The annual ISN (v.2) dataset (https://wwwbis.sidc.be/silso/
datafiles) is shown with the dotted red line. Approximate timing of the grand minima(Oort – OM, Wolf – WM, Spörer – SM, and Maunder – MM) are indicated with theblue letters.

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Article
Highlight on Young Scientists

Figure 2. Wavelet power spectrum (Morlet basis, k=6) of the annual sunspot number reconstruction shown in Figure 1. Black dots denote the period corresponding to the maximum power in the range of 8—16 years at each year.
The white lines indicate the cone of influence.

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urements of the relative abundance of radiocarbon Δ14C
in tree rings for the period since 970 BC (Brehm et al.,2021). Using updated models and independently known
archaeomagnetic reconstructions (e.g., Nilsson et al.,2014), these Δ14C data were converted into sunspot
numbers with the annual resolution (Usoskin et al.,2021), as shown in Figure 1. The new reconstruction
includes 85 individual Schwabe cycles, about 50 ofwhich are fairly or well resolved. This nearly triples the
known statistic (~36 cycles) based on telescopic observations. The cycles greatly vary in amplitude covering
the full range from low (three more grand minima ofOort, Wolf and Spörer are included in addition to theMaunder minimum, as indicated in Figure 1) to highactivity levels. The average length of solar cycles is10.8 years but vary significantly from cycle to cycle, as
shown in Figure 2. The cycles cannot be reliably determined during grand minima but they are clearly distinguishable for the periods of moderate and high activity.

References

A

Nilsson, A., R. Holme, M. Korte, N. Suttie, M. Hill
(2014) Reconstructing Holocene geomagnetic field variation: new methods, models and implications, Geophys. J. Intern., 198, 229, doi: 10.1093/gji/ggu120

basic analysis of the newly reconstructed solar
cycles for the last millennium has been performed
by Usoskin et al. (2021). This included the distributionof the cycle lengths that appears consistent with that ofthe direct sunspot data; confirmation of the grandminimum state of solar activity as a special mode of thesolar dynamo; and confirmation of the validity of theempirical Wadmeier’s rule (strong cycles tend to rise
faster) for larger statistic with high significance. The
SCOSTEP scientific community is welcome to perform
a more detailed investigation of the new dataset(available at http://cdsarc.u-strasbg.fr/viz-bin/cat/J/
A+A/649/A141).

Announcement
2

SCOSTEP/PRESTO Newsletter・Vol. 29

Arlt, R., Vaquero, J.M. (2020) Historical sunspot records, Living Rev Sol Phys, 17, 1. Doi: 10.1007/s41116020-0023-y
Beer, J., K.G. McCracken, and R. von Steiger (2012)
Cosmogenic Radionuclides: Theory and Applications in
the Terrestrial and Space Environments, Springer, Berlin.
Brehm, N., A. Bayliss, M. Christl, et al. (2021) Elevenyear solar cycles over the last millennium revealed byradiocarbon in tree rings. Nat. Geosci. 14, 10. Doi:
10.1038/s41561-020-00674-0
Eddy, J.A. (1976) The Maunder minimum, Science,
192, 1189, doi; 10.1126/science.192.4245.1189
Hathaway, D.H. (2015) The Solar Cycle. Living Rev.
Sol. Phys. 12, 4, doi: 10.1007/lrsp-2015-4

Usoskin, I.G. (2017) A history of solar activity overmillennia. Living Rev Sol Phys 14, 3, doi: 10.1007/
s41116-017-0006-9
Usoskin, I.G., S.K. Solanki, N.A. Krivova et al. (2021)
Solar cyclic activity over the last millennium reconstructed from annual 14C data, A stron. A strophys., 649,
A141, doi: 10.1051/0004-6361/202140711

Article

Article 2:

Diagnosing Atmospheric Planetary-Scale Waves
Through Multi-Station Approaches

TA

t first, we developed a dual-station approach todiagnose the zonal wavenumber of the underlying
dominant wave, which is called the phase differencetechnique [PDT, see He18a]. The principle is sketchedin Figure 1. Through cross-wavelet and Lomb-Scargle

Maosheng
He

spectral analyses, we implemented the PDT on meteor
wind collected from radar pairs at low-, mid-, and highlatitudes, as illustrated in Figure 2. The wavenumber
could also be determined through optimization, using
observations from an arbitrary number of radars. The
wavenumbers estimated through PDT using different
radar pairs were compared with those through the optimization using more than two radars, exhibiting consistency and evaluating the approaches [He20b, He21b].
According to the wavenumber estimations or priorknowledge, we assigned the most likely occurring
wavenumbers and estimated their wave amplitudes
through least-square regressions [He18a, He19, He21b].
In an evaluation, the least-square amplitudes exhibit
quantitative consistency with the results using winds
observed by the spacecraft ICON [He21b].

Meeting Report

he mesosphere-lower-thermosphere (MLT) region
is populated by intense global scale waves, but therelevant observations are sparse. Both balloons andspacecraft cannot routinely operate in MLT, and continuous observations are collected remotely by either optical instruments onboard satellites or radars on the
ground. These observations have been broadly used toinvestigate MLT waves. Most of these investigations are
based on single-station or -satellite approaches, andtherefore are subject to inherent spatiotemporal ambiguities [e.g., For12, He11]. Single-station approaches cannot determine the horizontal scale of waves. To conquer
this problem, we developed a series of multi-station
approaches.

Highlight on Young Scientists

Maosheng He1
1Leibniz-Institute of Atmospheric Physics at the Rostock University, Kühlungsborn, Germany
Email: he@iap-kborn.deCompared with single-station approaches, multistation approaches impose wavelength constraints
and allow diagnosing global-scale waves more determi-

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Figure 1. The principle of the phase difference technique [PDT, adjusted from the supporting information in
He18a]. The oscillations generated by a plane wave are coherent between any locations on the wave’s path. The
phase difference between any two locations is constant, proportional to the spacing multiplied by the aligned
wavenumber. Observational estimation of the phase difference provides a possibility for determining the aligned
wavenumber. To realize the possibility, we utilized the single- and long-wave assumptions. The single-wave assumption requires that only one wave exists at a given frequency and instant. To facilitate this assumption, in different circumstances, we trade-off differently the frequency and time resolutions by modulating the spectral analysis window size. The long-wave assumption requires the wavelength is longer than twice the station spacing tosatisfy Nyquist’s theorem, which can be relaxed slightly by assuming the zonal wavelengths of the underlying
waves are low order harmonics of 360° longitude.

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3Article
Highlight on Young Scientists

Figure 2. Meteor radar configurations used for multi-station analyses. Dots with the same color denote stations
that were paired for implementing the PDT. Crosses with the same color denote stations that were combined for
implementing the optimization and least-square regression.

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4

Figure 3. Waves diagnosed using multi-station approaches. Open circles denote lunar and solar tides. Solid dots
denote planetary waves of Rossby normal modes and Rossby-gravity waves. Triangles denote secondary waves
from nonlinear interactions between tides and planetary waves. Magenta symbols denote wave activities associated with SSWs. The regions in the dashed boxes in the left panel are zoomed into the right panels.

natively. We diagnosed a variety of novel wave activities, as summarized in Figure 3. In particular, many
wave activities were found or detailed during sudden
stratospheric warming events (SSWs), such as the enhancements of the Rossby normal modes [He20c], 12.4hour lunar tide [M2, see He18a, He18b], upper and lower sidebands (USB and LSB) of interactions between
planetary waves and tides [He19, He20a], interactions
between traveling and stationary planetary waves (PWs),
and 6-, 4.8-, and 4-hour migrating tides [He20b]. The
enhanced migrating tides quench at the SSW central day[He20b]. We noted that, in single-station analyses, M2
estimation is contaminated by a 12.4-hour LSB arisingfrom interactions between the 16-day wave and the 12hour migrating tide [He18b]. The interactions also produce an 11.6-hour USB. These LSB and USB have been
misinterpreted in some existing papers as two nonmigrating tides [SW1 and SW3, see He19]. Similar SW1like LSB and SW3-like USB also arise from interactionsof the 10-day wave, as observed during the Antarctic
SSW in 2019 [He20a]. Furthermore, three months before
this Antarctic SSW, we observed LSBs and USBs of

SCOSTEP/PRESTO Newsletter・Vol. 29

interactions between two quasi-2-day Rossby-gravity
waves and four solar migrating tides [He21a]. Besides
these meteorological activities, the climatology of PWs
and tides are also investigated using the multi-station
approaches [He19, He21a]. At the moment, we are systematically extending our works by implementing theapproaches on more meteor radar configurations andother ground-based observations, e.g., magnetometers[see For20], in broad ranges of frequency.
References[For12] J. M. Forbes and Y. Moudden. “Quasi-Two-Day
Wave-Tide Interactions as Revealed in Satellite
Observations”. In: Journal of Geophysical Research Atmospheres 117.12 (2012). ISSN:
01480227. DOI:10.1029/2011JD017114.
[For20] J. M. Forbes, M. He, A. Maute, and X. Zhang.
“Ultrafast Kelvin Wave Variations in the Surface Magnetic Field”. In: Journal of Geophysical Research: Space Physics 125.9 (2020),

21699402.

DOI:[He11] M. He, L. Liu, W. Wan, and Y. Wei. “Strong
Evidence for Couplings between the Ionospheric Wave-4 Structure and Atmospheric Tides”.
In: Geophysical Research Letters38.14 (2011),
pp.
2–7.
ISSN:
00948276.
DOI:
10.1029/2011GL047855.

[He18b] M. He, J. L. Chau, C. M. Hall, M. Tsutsumi, C.
Meek, and P. Hoffmann. “The 16-Day Planetary
Wave Triggers the SW1-Tidal-Like Signaturesduring 2009 Sudden Stratospheric Warming”.
In: Geophysical Research Letters 45.22 (2018),
pp. 12, 631–12, 638. ISSN: 19448007. DOI:
10.1029/2018GL079798.

[He20c] M. He, Y. Yamazaki, P. Hoffmann, C. M. Hall,
M. Tsutsumi, G. Li, and J. L. Chau. “Zonal
Wave Number Diagnosis of Rossby Wave-LikeOscillations Using Paired Ground-Based Radars”. In: Journal of Geophysical Research: Atmospheres 125.12 (2020). ISSN: 21698996.
DOI: 10.1029/2019JD031599.
[He21a] M. He, J. M. Forbes, G. Li, C. Jacobi, and P.
Hoffmann. “Mesospheric Q2DW Interactions
with Four Migrating Tides at 53°N Latitude:
Zonal Wavenumber Identification through DualStation Approaches”. In: Geophysical Research
Letters 48.8 (2021), e2020GL092237. ISSN:
19448007. DOI: 10.1029/2020GL092237.
[He21b] M. He et al. “Quasi-2-Day Wave in LowLatitude Atmospheric Winds as Viewed From
the Ground and Space during January–March,2020”. In: Geophysical Research Letters 48.13(2021).
ISSN:
19448007.
DOI:
10.1029/2021GL093466.

Meeting Report[He19] M. He and J. L. Chau. “Mesospheric Semidiurnal Tides and Near-12 h Waves Through Jointly
Analyzing Observations of Five Specular Meteor Radars from Three Longitudinal Sectors at
Boreal Midlatitudes”. In: Atmospheric Chemistry and Physics 19.9 (2019), pp. 5993–6006.
ISSN: 16807324. DOI: 10.5194/acp-19-59932019.

[He20b] M. He, J. M. Forbes, J. L. Chau, G. Li, W. Wan,
and D. V. Korotyshkin. “High-Order Solar Migrating Tides Quench at SSW Onsets”. In: Geophysical Research Letters 47.6 (2020), pp. 1–8.
ISSN:19448007. DOI: 10.1029/2019GL086778.

Highlight on Young Scientists[He18a] M. He, J. L. Chau, G. Stober, G. Li, B. Ning,
and P. Hoffmann. “Relations between Semidiurnal Tidal Variants through Diagnosing the Zonal
Wavenumber Using a Phase Differencing Technique Based on Two Ground-Based Detectors”.
In: Journal of Geophysical Research: Atmospheres123.8 (2018), pp. 4015–4026. ISSN:
21698996. DOI: 10.1002/2018JD028400.

Hocking.“Quasi-10-Day Wave and Semidiurnal
Tide Nonlinear Interactions during the Southern
Hemispheric SSW 2019 Observed in the Northern Hemispheric Mesosphere”. In: GeophysicalResearch Letters 47.23 (2020), 2020GL091453.
ISSN: 19448007. DOI: 0.1029/2020GL091453.

Articlee2020JA028488. ISSN:
10.1029/2020JA028488.

[He20a] M. He, J. L. Chau, J. M. Forbes, D. Thorsen, G.
Li, T. A. Siddiqui, Y. Yamazaki, and W. K.

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SCOSTEP/PRESTO Newsletter・Vol. 28

5Article

Highlight on Young Scientists 1:

Properties of High-Frequency Type II Radio Bursts
and Their Relation to the Associated Coronal
Mass Ejections

Highlight on Young Scientists

Ange Cynthia Umuhire1,2
1Rwanda Space Agency, Kigali, Rwanda.
2University of Rwanda, College of Science and Technology, Kigali, Rwanda

S

Meeting Reportolar radio bursts are often early indicators of space
weather events such as coronal mass ejections(CMEs). The high starting frequency implies shock formation closer to the solar surface, which has important
ramifications for the analysis of particle accelerationnear the Sun. In a recent study (Umuhire et al. 2021), we
determined the properties of 40 high frequency (≥150
MHz) type II bursts that occurred in solar cycle 24 (2010-2016) and the characteristics of the associated CMEs.
We found the CME heliocentric distances at the onset
time of metric type II bursts range from 1.16 to 1.90 solar radii (Rs). The study was also extended to 128 metric
type II bursts to include lower-starting-frequency eventsfor further analysis. The projected CME heights range
from 1.15 to 2.85 Rs. The lower starting frequency correspond to shocks forming at larger heights.

Figure 1 shows an example of a high-startingfrequency type II burst observed by the Green Bank
Solar Radio Bursts (GBSRB) spectrometer and its associated CME observed by STEREO-B/EUVI instruments.
The fundamental starting frequency of the type II burst
in the dynamic spectrum was 420 MHz at 17:35:00 UT.

Ange Cynthia
UmuhireThe ending frequency was 60 MHz at 17:40:30 UT. The
event was associated with a flare, which occurred at
N20E04 on the solar disk (see Cho et al., 2013, for details). The associated CME was at N20W90 in the STEREO-B Extreme Ultraviolet Imager (EUVI) field ofview (FOV). The CME-driven shock was observed in
EUV 64 seconds after the appearance of type II burst
corresponding to a height of 1.22 Rs.

W

e used STEREO/COR1, EUVI and SDO/AIA images to identify CME shocks close to the first appearance time of type II bursts and to minimize projection effects. We determined CME heights using both thewave diameter and leading edge methods (Gopalswamy
et al. 2013) for 117 of the 128 events for which theshock could be observed. We found that solar energetic
particles are accelerated very close to the coronal base.
Making use of type II bursts at different wavelengths, it
was found that the power law between the starting frequency and CME heights are consistent with the rapid
decline of density in the inner corona. The density drops
from lower corona to the interplanetary medium(Gopalswamy et al., 2009).

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6

Figure 1. (a) A high-starting-frequency type II burst. The dynamic spectrum was obtained by the Green Bank Solar Radio Burst Spectrometer (GBSRBS). The fundamental starting frequency was 420 MHz at 17:35:00 UT. The
high starting frequency implies the radio source closer to the solar surface, hence the associated CME originatingin the lower corona. (b) STEREO-B/EUVI 195 Å difference image shown by white arrow. The time of the image in(b) is close to the starting time of the type II burst. STEREO-B was located at E94 at the time of the eruption.

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Article
Highlight on Young Scientists
Meeting Report

Figure 2. (a) Scatter plot between the starting frequency f and the drift rate df/dt (absolute value) for the 40 highstarting frequency metric type II burst, the scatter plot represent a power law of the form | df/dt |〜 fꜫ with _ =1.19. (b) A similar plot for the 88 events with lower starting frequency, the power-law index (Ꜫ) increases to 1.49.
The combined set of 128 type II bursts in Figure (c) gives Ꜫ= 1.33. (d) The superposition of 10 data points reported in Gopalswamy et al. (2009) with 128 data points analyzed in this study. Ꜫ remains 1.33.

e also investigated how the high-frequency type II
bursts behave with respect to the power law nature of the drift rate spectrum of type II radio bursts (seeFigure 2). From the observations, the power-law exponent is the smallest at the highest frequencies, consistent
with the trend in the deviation from the universal drift
rate spectrum.
Acknowledgements

References

burst associated with the 2011 February 13 Coronal
Mass Ejection. Astrophys. J. 765, 148. DOI. ADS.
Gopalswamy, N., Xie, H., Mäkelä, P., Yashiro, S., Akiyama, S., Uddin, W., Srivastava, A.K., Joshi, N.C., Chandra, R., Manoharan, P.K., Mahalakshmi, K., Dwivedi,
V.C., Jain, R., Awasthi, A.K., Nitta, N.V., Aschwanden,
M.J., Choudhary, D.P.: 2013, Height of shock formationin the solar corona inferred from observations of type II
radio bursts and coronal mass ejections. Adv. Space Res.
51, 1981. DOI. ADS.
Gopalswamy, N., Thompson, W.T., Davila, J.M., Kaiser,
M.L., Yashiro, S., Mäkelä, P., Michalek, G., Bougeret, J.
-L., Howard, R.A.: 2009, Relation between type II bursts
and CMEs inferred from STEREO observations. Solar
Phys. 259, 227. DOI. ADS.

Announcement

The authors acknowledge NASA’s open data policy inusing SDO, SOHO, STEREO, and Wind data. ACU
acknowledges financial support from NASA-GSFC andSCOSTEP visiting scholarship program and administrative support from the Catholic University of America.
ACU also acknowledges the partial financial support
from the Swedish International Development cooperation Agency (SIDA).

Upcoming MeetingsW

Umuhire, A.C., Gopalswamy, N., Uwamahoro, J., Akiyama, S., Yashiro, S., Ma ̈kela ̈, P., 2021. Properties ofHigh-Frequency Type II Radio Bursts and Their Relation
to the Associated Coronal Mass Ejections. Sol. Phys.
296 (1), 27.

Cho, K.-S., Gopalswamy, N., Kwon, R.-Y., Kim, R.-S.,
Yashiro, S.: 2013, A high-frequency type II solar radio

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7Article

Highlight on Young Scientists 2:

Analysing CaII K Observations for Reconstructionsof Past Solar Irradiance Variations

Highlight on Young Scientists

Theodosios Chatzistergos1
1Max Planck Institute for Solar System Research, Göttingen, GermanyT

he Sun provides almost all of the external energy to
Earth, bearing the potential to affect Earth’s climate.
Measurements of the solar radiative energy flux at the
top of Earth’s atmosphere (solar irradiance) began in
1978. Climate studies require data for earlier periods,
which are provided by models.

S

Meeting Reportuch models reconstruct past solar irradiance by typically relying on sunspot observations, the longest
solar data available since 1600’s. Such observations,however, miss the bright magnetic features, faculae andnetwork, thought to be responsible for the secular irradiance changes.

I

nformation about faculae can be derived from fulldisc observations in the singly-ionized Calcium line,
CaII K. Despite CaII K observations are among the oldest systematic solar observations (since 1892), they havebeen largely unexplored for studies of long-term solar
variability.

T

Theodosios
Chatzistergos

database of over 300,000 CaII K observations from 38
observatories (Chatzistergos et al. 2020). We developed
an automatic procedure to correct for various artefacts in
the images and account for the non-linear response of thephotographic emulsion (Fig. 1). We have also determined the relation between the CaII K brightness and themagnetic field strength so to convert CaII K observations
to magnetograms (Chatzistergos et al. 2019) and constructed a plage-area composite record.

A

s a next step, we have adapted the SATIRE(Krivova et al. 2003) model to use magnetogramsreconstructed from CaII K images (Chatzistergos et al.
2021). We have reconstructed TSI variations from various CaII K archives over the period when direct TSI
measurements exist (Fig. 2) and showed that such data
can be used to recover past irradiance variations quite
accurately. This paves the way for using historical photographic CaII K archives for more accurate reconstructions of the irradiance variations back to 1892.

o take the full advantage of the potential of these
data, we have compiled the most comprehensive

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Figure 1. Exemplary observations from the Arcetri, Kodaikanal, Mt Wilson, and Kyoto sites. Shown are theraw positive observations (top) and the images processed and calibrated with our procedures (bottom).

8

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Article
Highlight on Young Scientists

Figure 2. Top: TSI variations reconstructed from Rome/PSPT Ca II K observations (red for daily and ciel for
81-day running mean). Also shown are the values from the PMOD TSI composite (black). Bottom left: Residuals between our reconstruction of TSI and the PMOD TSI composite (red for daily and ciel for 81-day running mean). The dashed blue line is a linear fit to the residuals, while the black dotted line is a line with notrend. Bottom right: distribution of residuals in bins of 0.05 Wm-2.
References

Krivova, N. A., S. K. Solanki, M. Fligge, and Y. C. Unruh. “Reconstruction of Solar Irradiance Variations in
Cycle 23: Is Solar Surface Magnetism the Cause?” Astronomy and Astrophysics 399 (2003): L1–4. https://doi.org/10.1051/0004-6361:20030029.

Upcoming Meetings

Chatzistergos, Theodosios, Ermolli, Ilaria, Solanki, SamiK., Krivova, Natalie A., Giorgi, Fabrizio, and Yeo, Kok
Leng. “Recovering the Unsigned Photospheric Magnetic
Field from Ca II K Observations.” Astronomy & Astrophysics 626 (2019): A114. https://doi.org/10.1051/00046361/201935131.

Meeting Report

Chatzistergos, Theodosios, Ilaria Ermolli, Natalie A.
Krivova, Sami K. Solanki, Dipankar Banerjee, Teresa
Barata, Marcel Belik, et al. “Analysis of Full-Disc Ca II
K Spectroheliograms - III. Plage Area Composite Series
Covering 1892–2019.” Astronomy & Astrophysics 639(2020):
A88.
https://doi.org/10.1051/00046361/202037746.

Chatzistergos, Theodosios, Natalie A. Krivova, Ilaria
Ermolli, Kok Leng Yeo, Sudip Mandal, Sami K. Solanki,
Greg Kopp, and Jean-Marie Malherbe. “Reconstructing
Solar Irradiance from Historical Ca II K Observations. I.
Method and Its Validation.” Astronomy & Astrophysics(in press) https://doi.org/10.1051/0004-6361/202141516
ArXiv:2109.05844 http://arxiv.org/abs/2109.05844.

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SCOSTEP/PRESTO Newsletter・Vol. 28

9Article

The 1st Summer School on Space Research, Technology & Applications for Young Scientists
and PhD Students

Highlight on Young Scientists

Meeting Report 1:

On behalf of SOC and LOC:
Rositsa Miteva1
1Institute of Astronomy with National Astronomical Observatory - Bulgarian Academy of
SciencesT

Meeting Report

he first edition of the summer school on Space research, technology and applications was held in the
National Astronomical Observatory – Rozhen, Bulgaria
from 5th to 11th July 2021 in a hybrid mode. Over 42(14 on-site and 28 online) participants from 20 different
countries attended the school. A versatile coverage of
topics from theoretical astrophysics to engineering andcomputing was offered to the students. The program wasorganized as morning online lectures and afternoon onsite practice sessions and was structured in three main
topics: Fundamental research (Theoretical astrophysics
and cosmology; Sun and space weather); Aerospacetechnologies; Space-related methods and applications(Earth observations; Machine learning). Five practicegroups were formed: Atmospheric measurements via
drone; Astrophotography; Forecasting of CME effects;
Machine learning; Sensors. At the end of the school,
each team presented the results from their practice work
led by an experienced mentor and on-site assistant. In

Rositsa
Mitevaaddition, each participant gave a short overview on their
PhD topic during a dedicated PhD session.

T

he summer school received financial support fromthe foundation America for Bulgaria, SCOSTEP,
Karoll foundation and British Council and was held under the auspices of the Ministry of Economy of Bulgaria.
Assistance was provided by the Institute of Astronomy Bulgarian Academy of Sciences, Bulgarian Science
Fund, and UK science & Innovation Network.

T

he initiative is planned to continue in future as anannual event in Bulgaria on space-related topics andbe open for PhD students and young scientists from allaround the globe. More details, open-access lectures,presentations and videos can be found at the summer
school web-site: https://bulgarianspace.online/spaceschoolbg-2021/ .

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Figures. Group photos of the on-site participants, organizers and youngsters in front of the 2-m telescope andits dome in NAO-Rozhen.

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Meeting Report 2:

Articlei4s – First Iberian Space Science Summer School

TeresaBarataAntonio
GuerreroHighlight on Young Scientists

Anna
Morozova

Rui
Pinto

Anna Morozova1, Teresa Barata1, Antonio Guerrero2, Rui Pinto3
1Instituto Astrofísica e Ciências do Espaço, University of Coimbra, Portugal
2Space Weather Research Group, Departamento de Física y Matemáticas, Universidad de Alcalá, Spain
3IRAP - Institut de Recherche en Astrophysique et Planétologie; Toulouse, FranceTN

ine lectures covered different space weather topics:
The Sun; Solar wind and interplanetary medium;
Magnetosphere; Ionosphere and Upper Atmosphere;

Lower atmosphere and ground effects; Climate Change.
All lectures were recorded, and the videos and the slides
were uploaded to the i4s Google Drive with passwordprotected access for school students, Lecturers and Mentors and lectures’ attendees.

The school was organized by IA (Portugal) and SWEUAH (Spain), with the support of ISWI andSCOSTEP, being in line with their aims in providing
training in the domain of Space Science.

Meeting Report

he i4s school 2021 (https://www.i4s-iberian-spacescience-summer-school.com/) was held between
July 26th and July 30th of 2021 on-line due to the
COVID19 pandemics using Zoom and Slack web services. The students of the i4s were almost equally distributed between the eastern (China, India, and Middle
Asia), Euro-African and western (N. and S. Americas).

Upcoming Meetings
Announcement

Figure. Zoom Group Photo of the participants of the i4s school 2021

SCOSTEP/PRESTO Newsletter・Vol. 28

11Article

Upcoming meetings related to SCOSTEPHighlight on Young Scientists

Conference

Date

LocationContact Information

The 30th IUPAP General Assembly

Oct. 20-22, 2021

Beijing, China

http://iupap-ga2020.cps-net.org.cn/

AGU Fall Meeting 2021

Dec. 13-17, 2021

New Orleans, LA,
USA

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

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

Feb. 21-25, 2022

Alibag, India

https://www.stp15.in/

EGU General Assembly 2022

Apr. 3-8, 2022

Vienna, Austria

https://www.egu22.eu/

COSPAR 2022

Jul. 16-24, 2022

Athens, Greece

http://ww.cosparathens2022.org/

AOGS 2022

Aug. 14-19, 2022

Melbourne,
Australia

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

Meeting Report

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

Houphouët Boigny
University, Abidjan, Côte d’Ivoire

AGU Fall Meeting 2022

Dec. 12-16, 2022

Chicago, IL, USA

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

IUGG 2023

In July, 2023

Berlin, Germany

https://www.iugg2023berlin.org/

AGU Fall Meeting 2023

Dec. 11-15, 2023

San Francisco, CA,USA

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

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

Upcoming Meetings
Announcement
12

SCOSTEP/PRESTO Newsletter・Vol. 29

ArticleAnnouncement 1:

VarSITI Review Papers Are Published in the Open
Access PEPS Journal

Katya
Georgieva

Highlight on Young Scientists

Kazuo
Shiokawa

Nat
Gopalswamy

Kazuo Shiokawa1, Katya Georgieva2, Nat Gopalswamy3
1Nagoya University, Japan
2Bulgarian Academy of Sciences, Bulgaria
3NASA Goddard Space Flight Center, USA(Associate Editors VarSITI Special Issue of Progress in Earth and Planetary Science)T

1.

SEE: D. Nandy, P. C. H. Martens, V. Obridko, S.
Dash and K. Georgieva, Solar evolution and extrema: current state of understanding of long-term
solar variability and its planetary impacts, PEPS,
8:40, 2021.
https://progearthplanetsci.springeropen.com/article
s/10.1186/s40645-021-00430-x

3.

ISEST/MiniMax24: J . Zhang, M. Temmer, N.
Gopalswamy, O. Malandraki, N.V. Nitta, S. Patsourakos, F. Shen, B. Vršnak, Y.-M. Wang, D. Webb,
M. I. Desai, K. Dissauer, N. Dresing, M. Dumbović, X.-S. Feng, S. G. Heinemann, M. Laurenza, N.
Lugaz, and B. Zhuang, Earth-affecting solar transients: a review of progresses in solar cycle 24,
PEPS, 8:56, 2021.
https://progearthplanetsci.springeropen.com/article
s/10.1186/s40645-021-00426-7

5.

ROSMIC: W. War d, W. War d, A. Seppälä, E.
Yiğit, T. Nakamura, C. Stolle, J. Laštovička, T. N.
Woods, Y. Tomikawa, F.-J. Lübken, S. C. Solomon,
D. R. Marsh, B. Funke, and D. Pallamraju, Role
Of the Sun and the Middle atmosphere/
thermosphere/ionosphere In Climate (ROSMIC): a
retrospective and prospective view, PEPS, 8:47,
2021.
https://progearthplanetsci.springeropen.com/article
s/10.1186/s40645-021-00433-8

T

he success of the VARSITI program was possible
due to the invaluable contributions from different
quarters: the International Space Science Institute(ISSI), the organizers of various symposia and workshops, the funding agencies that supported meeting andresearch activities, and above all the more than 1,000
scientists who focused their research efforts on VarSITI.

Announcement

2.

SPeCIMEN: S. Kanekal and Y. Miyoshi, Dynamics of the terrestrial radiation belts: a review ofrecent results during the VarSITI (Variability of the
Sun and Its Terrestrial Impact) era, 2014–2018,
PEPS, 8:35, 2021.
https://progearthplanetsci.springeropen.com/article
s/10.1186/s40645-021-00413-y

Upcoming Meetings

VarSITI: K. Shiokawa and K. Georgieva, A review of the SCOSTEP’s 5-year scientific program
VarSITI—Variability of the Sun and Its Terrestrial
Impact, PEPS, 8:21, 2021.
https://progearthplanetsci.springeropen.com/article
s/10.1186/s40645-021-00410-1

4.

Meeting Report

he Variability of the Sun and Its Terrestrial Impact(VarSITI) was the SCOSTEP’s 5-year international
program during 2014-2018. Four scientific projects
were carried out under the VarSITI program: (1) Solar
Evolution and Extrema (SEE), (2) International Study ofEarth-Affecting Solar Transients (ISEST/MiniMax24),(3) Specification and Prediction of the Coupled InnerMagnetospheric Environment (SPeCIMEN), and (4)Role Of the Sun and the Middle atmosphere / thermosphere / ionosphere In Climate (ROSMIC). Five review
papers that highlight the achievements of the VarSITI
program have now been published in a special issue ofthe Progress in Earth and Planetary Science (PEPS, open
access) . The papers are: https://www.springeropen.com/
collections/varsiti.

SCOSTEP/PRESTO Newsletter・Vol. 28

13

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. 29