OPS1 – Open Parallel Session
Talks
OPS1.1 Thu 7/11 17:30-18:30, room C2D – Almedina
Chair(s): Ilya Usoskin
Author(s): Julia Zink, Steffen Gaißer, Christoph Nöldeke, Sabine Klinkner
University of Stuttgart, Institute of Space Systems; SAT.IO; University of Stuttgart, Institute of Space Systems; University of Stuttgart, Institute of Space Systems
Abstract: The Flying Laptop small satellite, developed by the University of Stuttgart’s Institute of Space Systems, has been operational in Low Earth Orbit (LEO) since July 2017. Throughout its mission, the satellite has experienced several Single Event Upsets (SEUs) in onboard electronic components. This research investigates the frequency of SEUs from 2017 to 2024 in the satellite’s Static Random-Access Memory (SRAM) in relation to the satellite’s position, the corresponding McIlwain parameter (L-value) and effective cutoff rigidity.
The analysis revealed that SEU occurrences increase significantly in regions of L=3 or higher, and in areas with low cutoff rigidities. Additionally, the data indicates a noteworthy variation in SEU frequency in relation to the solar activity. Specifically, during periods of high solar activity, the frequency of SEUs decreased. This aligns with the decrease of galactic cosmic rays with increasing solar activity, indicating that most SEUs are caused by galactic cosmic rays and not by solar energetic particles.
This research provides valuable insights into the impact of space weather on satellites in LEO. This knowledge is crucial to mitigate severe space weather induced system failures or anomalies, which in turn can increase a spacecraft’s lifetime.
Author(s): Sandra C. Chapman, Thierry Dudok de Wit
CFSA, University of Warwick, UK; ISSI, Bern, Switzerland
Abstract: The variable solar cycle of activity modulates the overall level of space weather activity at earth, which in turn can have significant societal impact. The Hilbert transform of the sunspot number is used to map the variable length, approximately 11 year Schwabe cycle onto a uniform clock [1]. The clock is used to correlate extreme space weather seen in the aa index, the longest continuous geomagnetic record at earth, with the record of solar active region areas and latitudes since 1874. The clock reveals a sharp switch on and off of activity, with some of the most extreme events occurring close to the switch on/off, rather than at solar maximum. The switch on and off times can be directly identified from the sunspot number record, without requiring a Hilbert transform [2].
The clock shows that a clear switch-off of the most extreme space weather events occurs when the solar active regions move to within 15 degrees of the solar equator, from regions of high gradient in solar differential rotation which can power coronal mass ejections, to a region where solar differential rotation is almost constant with latitude. This overlaps with the onset of more moderate space weather events which coincide with 27 day solar rotation recurrences in the aa index, consistent with stable, persistent source regions [3]. This offers a physical explanation for the longstanding identification of a two component cycle of activity in the aa index. Model predictions of sunspot number can be translated into a clock which specifies the corresponding active region overall latitudes and the track of the extended cycle. Timing of the switch-off and on can be obtained via the clock for solar cycle predictions, providing quantitative estimates of future space weather risk, in particular, when the next switch on or off of activity will occur.[1] S. C. Chapman, S. W. McIntosh, R. J. Leamon, N. W. Watkins, Quantifying the solar cycle modulation of extreme space weather, GRL (2020) doi:10.1029/2020GL087795[2] S. C. Chapman, Charting the Solar Cycle, Front. Astron. Space Sci. – Space Physics, (2023) doi: 10.3389/fspas.2022.1037096[3] S. C. Chapman, T, Dudok de Wit, A solar cycle clock for extreme space weather, Sci. Rep. (2024) doi:10.1038/s41598-024-58960-5
Author(s): Kazumasa Iwai, Ken’ichi Fujiki, Yusuke Kagao, Haruto Watanabe, Takehara Daichi
ISEE, Nagoya University; ISEE, Nagoya University; ISEE, Nagoya University; ISEE, Nagoya University; ISEE, Nagoya University
Abstract: Interplanetary scintillation (IPS) is a radio scattering phenomenon generated by the disturbances in the solar wind. IPS observation has been one of the important tools for observing solar wind propagating in interplanetary space. Institute for Space–Earth Environmental Research (ISEE), Nagoya University have observed IPS to derive the solar wind velocity and density irregularities for several decades using multiple large radio telescopes at 327 MHz. The IPS data derived from this system have been also used to detect coronal mass ejections (CMEs). The fast-propagating CME can sweep the background solar wind and form a dense region in front of the CME. This region can significantly scatter the radio emission, that can be detected the IPS observation. We have detected CMEs that arrived at the Earth using the IPS observation such as generated May 2024.
The IPS data has been also used to improve the accuracy of the magnetohydrodynamic (MHD) simulation of the space weather forecast. The radio scintillation of each radio source was simulated by calculating the scattering of radio wave along the line of sight from the Earth to the radio source using the 3D density distribution of the heliosphere obtained from the MHD simulation results. This simulated IPS data can be compared with the observed IPS data. We have simulated several CME events that arrived at the Earth such as observed on early September 2017, early October 2021, and end of March 2023.
Now, a new project to develop the next-generation solar wind observation system is in progress. We consider a new ground-based radio observation system at 327 MHz by constructing a 2D flat phased-array antenna system consisting of multiple dipole antennas, and installing digital beam forming devices. The multidirectional simultaneous radio scintillation observation using this system enables the solar wind observation 10 times as much as the conventional radio instruments have been done. A small scale array system is under construction as a phase-I project. This array will be expanded in the coming phase-II stage.
Author(s): Jean Lilensten, Jean-Luc DAUVERGNE, Emmanuel Beaudoin, Christophe Pellier, Marc Delcroix, Mathieu Vincendon
Univ. Grenoble-Alpes, CNRS, IPAG, 38000 Grenoble, France; Société de Planétologie des Pyrénées (S2P) 5 rue Gazan, 75014 Paris, France; Université Paris-Saclay, LPS (UMR8502), 510 Rue André Rivière, 91400 Orsay, France; Commission des Observations planétaires, Société Astronomique de France, 3, rue Beethoven, 75016 Paris, France; Commission des Observations planétaires, Société Astronomique de France, 3, rue Beethoven, 75016 Paris, France; Institut d’Astrophysique Spatiale, Université Paris Saclay, Orsay, France
Abstract: On November 17, 2020, a 3,000 km long cloud was observed at Mars following a joint effort by a group of amateur and professional astronomers (Lilensten et al., 2021). Frenchmen Christophe Pellier and Emmanuel Beaudoin followed a huge cloud structure located at the terminator for 3 hours in a row through different filters. The images obtained show the formation emerging from the night, clearly separated from the terminator. Its evolution was followed until the sun rose over the terrain beneath the cloud. The cloud dissipates shortly afterwards. What was observed here is atypical in two respects: not only is the cloud complex gigantic in relation to the planet, it is also located at an altitude of 92 km, at the gateway to the interplanetary void.
Detailed analysis of the photometric data showed this atypical cloud is probably made of CO2 ice and that cosmic rays play a role in the nucleation of ice crystals at this altitude, especially as the structures observed are on the edge of a magnetic zone.
This cloud is therefore strongly linked to Mars space weather.
However, the initial aim of the program was fairly different: it was to detect polar aurorae on Mars, following the prediction made in Lilensten et al., 2015. This hypothesis was seriously considered to explain the observation of November 17, 2020, but then dismissed because the structures observed cast a shadow on the ground. Moreover, the phenomenon tends to occur at the edge of areas where Mars’ magnetic field is most disturbed, and solar activity was low that day. On the other hand, a review of previous amateur observations published in 2015 by Sanchez et al. shows that the 2012 observations they report take place above this magnetic zone and coincide with coronal mass ejection episodes. We are therefore potentially dealing with two different phenomena.
Both phenomenon – high altitude clouds and aurorae – are observable from the Earth while the planets are in opposition. This occurs about every 2 years. We were lucky in November 2020 but the weather conditions were unfavorable in 2022. We are now preparing for the next opposition (January 16, 2025). The best periods for these observations are around November 15-20, 2024, around Christmas, and the first ten days of March 2025. In this lecture, we will therefore give a call for participation to this program over the 5 Earth continents, so that whatever the local time and the local weather, observers can help either to better characterize these clouds and/or to make the first observation of the Mars visible aurorae.
OPS1.2 Fri 8/11 09:00-10:15, room C2A – Mondego
Chair(s): Ilya Usoskin
Author(s): Janet Machol, James Mothersbaugh III, Donald Woodraska, Thomas Eden, James Negus, Frank Eparvier, Thomas Woods, Andrew Jones, Edward Thiemann, Ann Marie Mahon, Martin Snow, William McClintock
University of Colorado CIRES and NOAA NCEI; University of Colorado CIRES and NOAA NCEI; University of Colorado LASP; University of Colorado LASP; University of Colorado CIRES and NOAA NCEI; University of Colorado LASP; University of Colorado LASP; University of Colorado LASP; University of Colorado LASP; University of Colorado CIRES and NOAA NCEI; SANSA; University of Colorado LASP
Abstract: Solar X-ray and extreme ultraviolet (EUV) science-quality solar irradiance measurements from GOES spacecraft are critical for space weather operations and are also provided publicly for scientific use. These measurements, at cadences of 1 to 10 seconds, have been made continuously since 1975 for soft X-rays with the X-Ray Sensor (XRS), and since 2006 at EUV wavelengths with the Extreme Ultraviolet Sensor (EUVS). The Extreme Ultraviolet and X-ray Irradiance Sensors (EXIS) on GOES-R (GOES-16 through -19) have new XRS and EUVS instrument designs with better calibration and more capabilities than earlier GOES irradiance instruments. NOAA NCEI provides a variety of new and re-calibrated science-quality data products including irradiances at various cadences, modeled EUV spectra, flare summaries, and flare locations, for both current and earlier satellites. We will discuss the measurements, data products, and applications and show example measurements from the May 2024 geostorm period.
Author(s): Elsayed R. Talaat
NOAA
Abstract: The National Oceanic and Atmospheric Administration (NOAA) Office of Space Weather Observations will support the forecasting of space weather events, such as geomagnetic storms, ionospheric disturbances, solar wind, solar flares, and coronal mass ejections (CMEs), in addition to providing backbone measurements necessary for research. The Space Weather Observations Programs Division, a joint NOAA and National Aeronautics and Space Administration (NASA) office, is managing both the Space Weather Follow-On (SWFO) and Space Weather Next (SW Nextt) programs.
The SWFO program will provide operational coronal imagery and in situ solar wind measurements to the science community and to space weather information users. In this talk, we provide an update on the status of the Compact Coronagraph 1 (CCOR-1) and the other space weather instrumentation onboard the Geostationary Operational Environmental Satellite 19 (GOES-19) launched on June 25, 2024. We will also discuss the status of the SWFO-Lagrange 1 (SWFO-L1) observatory at the Sun-Earth Lagrange 1 point (L1) as it finalizes testing ahead of its planned 2025 launch. SWFO-L1 carries a second coronagraph (CCOR-2) and a suite of in-situ instrumentation that will provide upstream observations needed for operational and scientific applications.
The projects under the SW Next program will provide for the continuity of the SWFO-L1 mission, through the L1 Series project, as well as other new and necessary multi-point observations into the 2030s. The SW Next program is closely collaborating with the European Space Agency (ESA) on the Vigil mission (2031), which will carry NOAA’s Compact Coronagraph 3 (CCOR-3) as part of its extensive payload and will provide measurements from the Lagrange 5 (L5) point. Furthermore, future SW Next missions include observations at Geostationary Orbit (GEO) and Low Earth Orbit (LEO) with space weather measurements improving on those provided by the ongoing Geostationary Operational Environmental Satellites (GOES)–R Series and the historic Polar Orbiting Environmental Satellites (POES) programs. All measurements from GOES, SWFO, and SW Next will be made available through the Space Weather Prediction Center (SWPC) and the National Centers for Environmental Information (NCEI) and are expected to enhance the accuracy and timeliness of National Weather Service (NWS) forecasts significantly. They will also provide unprecedented opportunities for research and applications in academia and industry.
Author(s): MAYANK KUMAR, Kris. Murawski, B. Kuzma, E.K.J. Kilpua, S. Poedts, Robertus Erdelyi
UNIWERSYTET MARII CURIE-SKŁODOWSKIEJ, LUBLIN, POLAND AND UNIVERSITY OF HELSINKI, HELSINKI, FINLAND; UNIWERSYTET MARII CURIE-SKŁODOWSKIEJ, LUBLIN, POLAND; Shenzhen Key Laboratory of Numerical Prediction for Space Storm, Institute of Space Science and Applied Technology, Harbin Institute of Technology, Shenzhen, People’s Republic of China,; UNIVERSITY OF HELSINKI, HELSINKI, FINLAND; KU LEUVEN, BELGIUM; Department of Astronomy, E ̈otv ̈os Lor ́and University, P ́azm ́any P ́eter s ́et ́any 1/A, H-1112 Budapest, Hungary
Abstract: This paper offers a fresh perspective on solar chromosphere heating and plasma outflows, focusingon the contribution of waves generated by solar granulation. Utilizing the 2.5-D numerical experiment in the partially ionized lower solar atmosphere, we investigate the dissipation of these waves and their impact on plasma outflows and chromospheric heating via ion-neutral collisions. Employing the JOint ANalytical Numerical Approach (JOANNA) code, we adopt the two-fluid model equations, examining partially ionized hydrogen plasma dynamics, including protons, electrons, and neutrals, coupled through ion-neutral collisions. Our investigation focuses on a quiet region within the solar chromosphere, characterized by gravitational stratification and magnetic confinement by an initially set single magnetic arcade. The primary source of the waves is the solar convection beneath the photosphere. A fraction of the energy of such waves dissipates due to ion-neutral collisions, releasing thermal energy that heats the chromosphere plasma. Notably, this is accompanied by upward-directed plasma flows. Finally, we conclude that wave dissipation due to ion-neutral collisions in the two-fluid plasma model induces chromosphere heating and plasma outflows.
Author(s): Sergio Dasso, Christian Gutierrez, Pascal Démoulin, Miho Janvier
LAMP – IAFE (UBA/CONICET), Buenos Aires, Argentina.; LAMP – IAFE (UBA/CONICET), Buenos Aires, Argentina.; Observatory of Paris, Meudon, France; STEC – European Space Agency, The Netherlands
Abstract: Plasma coming from different solar regions can create different interplanetary conditions when access to the heliosphere.
The interior of coronal holes (CHs) are sources for fast solar wind, which typically is preceded by slow solar wind, creating stream interaction regions (SIRs). SIRs can have several consequences in the medium, such as producing shock waves; accelerating particles; changing the direction of the interplanetary magnetic field; increasing its modulus as well as the plasma density and temperature, mainly as consequence of the plasma compression. SIRs also change the conditions for propagation of galactic cosmic rays (GCRs) in the heliosphere, causing Forbush decreases (FDs).
A detailed analysis of the structure of SIRs and of consequente FDs, applying an original normalized superposed epoch technique to a large samples of events, will be shown here. Finally, for getting insight of most relevant physical processes, we will make a compararive analysis between FDs produced by SIRs respect to the ones produced by interplanetary coronal mass ejections.
Author(s): Reinhard Friedel
NASA HQ Heliophyscis Division
Abstract: Within the Heliophysics Division (HPD) of NASA’s Science Mission Directorate (SMD), Orbital Debris – Space Situational Awareness (OD-SSA) has been stood up as an “activity” in early 2021, with OD-SSA becoming an official part of HPD’s Space Weather Program in Fiscal Year 2024. OD (anthropogenic debris, micro meteorites and dust) are now included in HPD’s definition of the Space Working Environment – defined as all parts of the space environment that “affect human activities in space”.
This talk will present an overview of the OD-SSA activities in HPD, past and present, including:
Addressing the measurement gap of <1cm OD (instrument development concepts and flight opportunities)
Mission Design Lab activities on a dedicated small OD characterization mission
New OD science – signatures of objects moving through a space plasma
Posters
Posters II Display Thu 7/11 – Fri 8/11, room C1A – Aeminium
Authors in attendance: Thu 7/11 10:15–11:30, 15:15-16:15; Fri 8/11 10:15–11:30
Author(s): Gamal Zayed, Yehea Ismail
Center of Nanoelectronics and Devices (CND), The American University in Cairo; Center of Nanoelectronics and Devices (CND), The American University in Cairo
Abstract: Accurate weather prediction and understanding of space weather phenomena are critical for safeguarding society and infrastructure against the impacts of severe atmospheric events. Doppler radar systems serve as essential tools for terrestrial weather forecasting and space weather monitoring, providing crucial insights into precipitation, wind patterns, and ionospheric disturbances.
This study focuses on advancements in local oscillator design tailored for Doppler radar applications, with implications for both terrestrial weather forecasting and space weather monitoring. Leveraging the UMC65 process technology with a supply voltage of 1.4 V, our design targets an oscillation frequency of 13 GHz to capture detailed atmospheric dynamics and ionospheric disturbances.
Critical to the design is the control of phase noise, with stringent specifications of less than -100 dBc/Hz at a frequency offset of 1 MHz. This ensures minimal signal distortion and high sensitivity in detecting Doppler shifts and ionospheric irregularities.
Additionally, power efficiency and signal integrity are prioritized, aiming for a peak differential output swing of more than 1 V and a maximum current consumption of less than 5 mA. These design considerations are essential for sustainable operation in remote or mobile radar installations, crucial for both terrestrial and space weather monitoring applications.
Furthermore, the design incorporates multi-finger transistor configurations, optimizing current-carrying capacity and stability while adapting to varying environmental conditions. By pushing the boundaries of local oscillator performance, our research contributes to advancing the capabilities of Doppler radar technology in understanding atmospheric dynamics and monitoring space weather phenomena.
In summary, the design approach to local oscillator design bridges the gap between terrestrial weather forecasting and space weather monitoring, facilitating more accurate predictions and enhancing our understanding of atmospheric and ionospheric processes. We look forward to presenting our findings and fostering discussions at the ESWW-2024 workshop to advance research in atmospheric and space science.
Author(s): C. Soneira-Landín
Complutense University of Madrid
Abstract: Since their discovery in 1912, cosmic rays have been an invaluable source of information about the distant universe, constituting one of the pillars of the so-called multi-messenger astronomy. They also act as penetrating radiation, providing information about near-Earth space and solar activity. In order to deepen our knowledge of cosmic rays, a new family of detectors called Trasgos has been proposed. These high granularity tracking devices employ Resistive Plate Chambers (RPCs) to detect ionizing secondary cosmic rays in a plug-and-play philosophy. The 0.1 m² small size Trasgo presented here includes pressure, temperature, and humidity sensors, as well as built-in rate monitoring software and hit maps. The detector performance and calibration procedures are outlined, along with results from measurements and preliminary analyses. As an example of its scientific potential, the first measurements during a Forbush decrease (FD) are presented.
Author(s): Ilya Usoskin, Gennady Kovaltsov, Alexandar Mishev
University of Oulu, Finland; Ioffe Physical-Technical Institute; University of Oulu, Finland
Abstract: Omnipresent galactic cosmic rays and sporadic solar energetic particles form the main source of air ionization in the low and middle atmosphere, that is important for various chemical and physical effects in the atmosphere. It is crucially important to model this process correctly for different conditions. One of the most commonly used atmospheric ionization models is CRAC:CRII (Cosmic-Ray Atmospheric Cascade: application to CRII) which was developed as the first full-physics model in 2004 – 2006 (version 1) and significantly improved by including the upper stratosphere in 2010 – 2011 (version 2). Here, we present a new version 3 of the CRAC:CRII model which offers a higher accuracy for the middle-upper atmosphere and lower-energy cosmic rays. This is particularly important for studies of the atmospheric effects of solar energetic particles. The model provides detailed lookup tables of the ionization yield function for the primary cosmic ray protons and α-particles (the latterrepresenting also heavier cosmic-ray species) and can be converted with any type of the energy spectrum and composition of cosmic rays.
Author(s): C. Soneira-Landín
Complutense University of Madrid
Abstract: Cosmic ray detectors are one of the basic tools for the study of Space Weather
phenomena. In particular, the Trasgos constitute a family of detectors that combine
high angular resolution, their sensitivity to bundles of particles and to ability of
separate muons from electrons. The new miniTrasgo detectors offer the same
performance, in a smaller size and at a more a affordable cost. Two miniTrasgos are
already operational in Madrid and Warsaw and before the end of the year two new
detectors will be installed in Puebla and Monterrey, in Mexico. All of them working
in a network will allow continuous monitoring of the terrestrial sky, opening a new
way of measuring Space Weather phenomena.
OPS1-p05 Historical geomagnetic observations from the Netherlands during the Carrington event (1859)
Author(s): Kasper van Dam, Ciaran Beggan, Eelco Doornbos, Bert van den Oord
KNMI; BGS; KNMI; KNMI
Abstract: The Carrington event is the best known example of an extreme geomagnetic storm, often cited to discuss space weather risks for modern infrastructure. Observations including auroral sightings, magnetometer records and anecdotes of impacts on telegraph systems have been widely shared before, but none of these have included observations from the Netherlands. Geomagnetic observations taken in Utrecht and Den Helder during the Carrington event were digitised from KNMI’s yearbook of 1859, and compared to magnetograms from London. Conversion factors from Den Helder have been used in combination with the diurnal variation measurements to estimate the conversion factors of the Utrecht data, which are missing in the yearbooks from that period. Both independent datasets from the United Kingdom and the Netherlands are consistent with each other. The correlation between the declination measurements made in London is strong with correlation coefficients larger than 0.7 for the Utrecht data and larger than 0.9 for the Den Helder data. The horizontal intensity measurements compared to Den Helder data give correlation values larger than 0.8 but the observations from Utrecht match less well. The coherent registration of two short-lived features may suggest that the agreement between the datasets is also valid on timescales shorter than the three times per day cadences, indicating that the magnetograms from the United Kingdom may be used for impact assessment studies for Dutch vital infrastructure. Further research including the digitisation of Dutch historical magnetograms is needed to investigate whether this coherence also holds at the minute timescale.
Author(s): Joachim Raeder
UNH Space Science Center
Abstract: We investigate the hypothesis that geomagnetic storms affect
local weather. We use the Disturbance Storm-Time (Dst) index to
identify storm days by requiring that Dst reaches a value below
a given threshold (Dst storm values are negative.) We then use
The Open-Meteo Historical Weather API to obtain local weather
data for a number of stations across the continental US for the
period 1970-2022. For each Day Of Year (DOY) we calculate the
average (AV) and the standard deviation (STD) for a number of
weather variables over the 1970-2022 period. For each SD we then
calculate the anomaly as the difference between AV and the
actual value on a storm day, and average those over the interval
and over the stations. Those values are normalized to the STD to
make them easier to interpret. We find that there is no
significant storm effect for wind speed, air pressure, and
precipitation. However, there are significant anomalies for air
temperature and direct radiation. There are also significant
regional difference of the anomalies for all of the variables
tested.
Author(s): Valentina Zharkova
Northumbria University, Newcastle, NE1 8ST, UK
Abstract: In this paper, we investigated the Oceanic Niño Index (ONI), for simplicity called in
this paper an El Nino Southern Oscillation (ENSO) index in 1950-2023 by applying
the wavelet spectral transform and the IBM SPSS correlations analysis. ONI follows
the three months’ current measurements of the average temperature of the sea
surface in the East-Central tropical part of the Pacific Ocean nearby the international
line of the date change over the average sea surface temperature over the past 30
years. The ENSO index is found to have a strong (>87%) correlation with the Global
Land-Ocean Temperature (GLOT). The scatter plots of the ENSO-GLOT correlation
with the linear and cubic fits have shown that the ENSO index is better fit by the
cubic polynomial increasing proportionally to a cubic power of the GLOT variations.
The wavelet analysis allowed us to detect the two key periods in the ENSO (ONI)
index: 4 – 5 years and 12 years. The smaller period of 4.5 years can be linked to the
motion of tectonic plates while the larger period of 12 years is shown to have a
noticeable correlation of 25% with frequencies of the underwater (submarine)
volcanic eruptions in the areas with ENSO occurrences. Not withholding any local
terrestrial factors considered to contribute to the ENSO occurrences, we investigated
the possibility of the volcanic eruptions causing ENSO to be also induced by the tidal
forces of Jupiter and Sun showing the correlation of the underwater volcanic
eruption frequency with the Jupiter-Earth distances to be 12% and with the Sun-
Earth distances, induced by the solar inertial motion, in January, when the Earth is
turned to the Sun with the southern hemisphere where the ENSO occurs, to become
15%. Hence, the underwater volcanic eruptions induced by tidal forces of Jupiter
and Sun can be the essential additional factors imposing this 12 year period of the
ENSO (ONI) index variations.
Author(s): Patrik Pinczes, Attila Hirn, Gabor Albrecht, Boglarka Erdos, Jonathan P. Eastwood, Dorottya Milankovich, Balazs Zabori
HUN-REN Centre for Energy Research; HUN-REN Centre for Energy Research; HUN-REN Centre for Energy Research; HUN-REN Centre for Energy Research; Imperial College London; C3S LLC; HUN-REN Centre for Energy Research
Abstract: The development of a space weather instrument suite, called RadMag, was initiated in the HUN-REN Centre for Energy Research a couple of years ago. The major goal of the development is to combine tools for radiation and magnetic field measurements into a single versatile payload, which could be utilized aboard different satellite platforms and in different type of orbits. A compact version of RadMag (RM-S) was flying on board the Hungarian 3-unit technology demonstration CubeSat RADCUBE. For this version, the magnetometer was provided by Imperial College London, and the boom mechanism by Polish company Astronika. The CubeSat platform was provided by the C3S LLC, Hungary. RADCUBE was conducted under the auspices of the European Space Agency CubeSat programme, and it was launched in August 2021 to a sun-synchronous low-Earth polar orbit. Payload commissioning started on the 29th of October 2021, and the nominal mission lasted until 2nd May 2022. The radiation monitor part of RM-S comprises two silicon detector telescopes to measure the flux of energetic protons, electrons and heavier ions. In our talk we introduce the instrument, describe the Level-0, -1, -2 data products and present the flight data measured with the RM-S radiation monitor during commissioning and the nominal mission. A brief outlook will be also given on the recent updates of the general RadMag development with focus on radiation monitoring.
Author(s): Levente Király, Adel Malatinszky, Attila Hirn, Balazs Zabori
Budapest University of Technology and Economics; HUN-REN Centre for Energy Research, Eötvös Loránd University; HUN-REN Centre for Energy Research; HUN-REN Centre for Energy Research
Abstract: The Space Research Department of the HUN-REN Centre for Energy Research has been involved in a number of experiments to study the characteristics of the radiation field on board stratospheric research balloons and a sounding rocket during different geomagnetic conditions (TECHDOSE on board BEXUS-14 in 2012, REM-RED on board REXUS-17 in 2015, and RADMOS on board HEMERA in 2022). The measurements were performed with detectors of direction-dependent geometric sensitivity (Geiger-Müller counters in different orientations and silicon detector telescopes) and they shed light on the direction-dependent properties of the secondary radiation field. We introduce the measurement setup and the environmental conditions during the flights. A comparative analysis of the results will be given, with main emphasis of the measured Pfotzer-maxima and its correlation with the Kp index. A brief outlook is given to the measurement setup of the radiation experiment TELLER to be developed by a group of students from the Budapest University of Technology and Economic for the REXUS-34 sounding rocket flight scheduled in March 2025 that will allow a more precise study of the directional dependence of the space radiation environment in the lower atmosphere.
Author(s): Nikolay Nikonov, Cristina Consolandi, Veronica bindi, claudio corti
university of hawaii; university of hawaii; university of hawaii; university of hawaii
Abstract: The Pacific Ocean presents a significant gap in the global Neutron Moni- tor (NM) network for
Solar Neutron Particles (SNP) and high energy Galactic Cosmic Rays (GCR) detection. To address
this issue, we are redeploying the Haleakala Neutron Monitor (HLEA) on the island of Maui. This
strategic location in the Pacific Ocean at a high altitude on Haleakala mountain, offers unique
advantages for SNP detection. The old HLEA detectror was estab- lished in 1991 but was
subsequently decommissioned in 2006 due to funding constraints. The reinstatement of HLEA will
extend the ground coverage of SNPs and GCRsn, enhancing the global NM network, and
contributing to a deeper understanding of high-energy particle interactions. Present status of the
HLEA redeployment will be presented.
Author(s): Arik Posner, Olga Malandraki, Kostas Tziotziou, Michalis Karavolos, Fanis Smanis, Bernd Heber, Henrik Droege, Patrick Kuehl
NASA Headquarters, Washington DC, USA/NASA Johnson Space Center, SRAG, Houston TX, USA; National Observatory of Athens, IAASARS, Athens, Greece; National Observatory of Athens, IAASARS, Athens, Greece; National Observatory of Athens, IAASARS, Athens, Greece; National Observatory of Athens, IAASARS, Athens, Greece; Christian-Albrechts-Universitaet zu Kiel, Germany; Christian-Albrechts-Universitaet zu Kiel, Germany; Christian-Albrechts-Universitaet zu Kiel, Germany
Abstract: We report on an attempt towards improving the HESPERIA Relativistic Electron Alert System for Exploration (REleASE) forecasting system by including the occurrence of a Type-III radio burst as a precondition for a HESPERIA REleASE forecast. HESPERIA REleASE forecasts are based on the detection of early arrival of near-relativistic electrons ahead of more hazardous protons from Solar Energetic Particle (SEP) events. The goal is to provide astronauts on future Lunar or Mars mission sufficient advance warning to reach a radiation shelter to minimize radiation dose exposure. To improve the HESPERIA REleASE forecast capabilities, we have developed a new system that a) automatically identifies Type III radio bursts that are associated with electron beams accelerated in solar eruptive events, and b) sets a condition of the occurrence of a Type-III radio burst associated with significant SEPs (with proton fluxes above 0.1 cm-2 s-1 sr-1 MeV-1), thus adding independent evidence of particle escape from the Sun, with the aim of reducing known sources of false-alarms of the existing system. The HESPERIA REleASE+ system, which takes advantage of availability of real-time solar radio observations from STEREO-A/SWAVES during its approach close to Earth and on its way to L4, has now been incorporated and running in the HESPERIA framework (https://hesperia.astro.noa.gr). We discuss the techniques used for the automatic detection of Type-III radio bursts, the determination of selection criteria for Type-III bursts that are candidates for solar proton events in the Earth-moon system, an assessment of the HESPERIA REleASE+ performance and representative results of the combined system
Author(s): Fan Lei, Joey O’Neill, Ben Clewer, Paul Morris, Clive Dyer, Keith Ryden
Surrey Space Centre, University of Surrey; Surrey Space Centre, University of Surrey; Surrey Space Centre, University of Surrey; Surrey Space Centre, University of Surrey; Surrey Space Centre, University of Surrey; Surrey Space Centre, University of Surrey
Abstract: Under UKSA and ESA funding, we are developing new detection techniques based on the Cherenkov radiation for measuring the solar and trapped relativistic, i.e. > 300 MeV, protons. Over the past year we have established the baseline requirements; developed a modular baseline design and evaluated the performance of different configurations; a breadboard implementation has been completed and a beam test campaign at the TRIUMF proton irradiation facility is to take place in mid-July. We will report on all these activities and the preliminary results achieved so far.
Author(s): Mario M. Bisi, Michael Garrett, Marco Martorella, Simon Garrington, Biagio Forte, Robert Beswick, Richard A. Fallows
UKRI STFC RAL Space, UK; JBCA, University of Manchester, UK; University of Birmingham, UK; JBCA, University of Manchester, UK; University of Bath, UK; JBCA, University of Manchester, UK; UKRI STFC RAL Space, UK
Abstract: RASOR: Radio Astronomy and Space Observation Research Facility, a potential new facility operating at wide-band radio frequencies (10s MHz to several GHzs) to provide unique observational and monitoring capabilities (high angular/temporal resolution) for frontier science in space weather, cosmology, astrophysics, and also to address strategic requirements for the prediction of adverse space-weather events and characterisation of assets/debris in orbit – tackling many areas across the Earth’s space environment. This advancement, when realised, represents a major step-change in current capabilities (e.g. 5x e-MERLIN, 10x SKA resolution), addresses up to 13 of the 23 of the STFC Science Challenges, looks at UN Sustainability Development Goals (SDGs), and will have substantial near- and long-term direct economic and societal impacts beyond research for the UK and further afield.
This would be a truly multi-disciplinary/interdisciplinary world-class project on UK soil, going beyond current and planned capabilities, and working as a standalone infrastructure and/or with international facilities (SKAO/LOFAR/VLBI). It would be able to support a very-broad, highly-engaged, diverse UK scientific community, providing direct access to high-resolution, rapid-response radio imaging and dedicated space-weather monitoring, unavailable anywhere else, and feed into Met Office space-weather monitoring requirements across the Sun-Earth chain.
This is a project opportunity submitted for UKRI/STFC infrastructure funding based on a two-year preliminary project, followed by a four-year full roll-out. Here, we will give an overview of RASOR with a focus on space weather and the space environment, an overview of the project plan, and where we are in terms of obtaining funding for the future.
Author(s): Vitória Marques da Silva, Marcelo Araujo da Silva
ABC Federal University; ABC Federal University
Abstract: This research project aims to study the reliability of the Rover Perseverance landing on Mars using the Monte Carlo Process (MCP) responsible for generating projects through random samples that will be processed to determine the probability of failure, together with the Method of Generalized Reduced Gradient (GRG), which consists of using optimization techniques to determine the highest probability of failure of a mathematical model that represents the mechanical process of force balance during landing, tools that can also be applied in space geophysics. The Excel Solver for MCP and GRG and the Python libraries for MCP were used to compare with the results already obtained with the solver. The acquired data was discussed in order to understand and study the Rover Perseverance landing on Mars from a reliable point of view.
Keywords: Optimization, Reliability, Rover Perseverance, Probability.
Author(s): Alexandre Winant, Viviane Pierrard, Edith Botek
Royal Belgian Institute for Space Aeronomy; Royal Belgian Institute for Space Aeronomy; Royal Belgian Institute for Space Aeronomy
Abstract: When high-energy particles originating from space penetrate the atmosphere, they may interact with atoms and molecules, initiating secondary particle air showers propagating toward the ground. They result in atmospheric ionization and contribute to the radiation dose at lower altitudes. We uses the GEANT-4 based Atmospheric Radiation Interaction Simulator (AtRIS) toolkit to compute those quantities in the Earth’s atmosphere. We take advantage of the unique Planet Specification File (PSF) of the Atmospheric Radiation Interaction Simulator (AtRIS) to investigate the effect of the state of the atmosphere on the resulting induced ionization and absorbed dose rates from the top of the atmosphere (at 100 km) down to the surface. The atmospheric profiles (density, pressure, temperature, and composition) are computed with the NRLMSISE-00 model at various latitudes and every month of 2014, corresponding to the last maximum of solar activity. The resulting ionization and dose rates present different profiles that vary with latitude in the atmosphere, with the relative difference between equatorial and high latitudes ionization rate reaching 68% in the Pfotzer maximum. We obtain differences up to 59% between the equator and high latitudes observed at commercial flight altitudes for the radiation dose. Both ionization and absorbed dose rates also feature anti-phased seasonal variations in the two hemispheres throughout 2014. Based on those results, we computed global maps of the ionization and dose rates at fixed altitudes in the atmosphere by using pre-computed maps of the effective vertical cutoff rigidities and the results of three AtRIS simulations to consider the effect of latitude. While sharing the same general structure as maps created with a single profile, those new maps also show a clear asymmetry in the ionization and absorbed dose rates in the polar regions.
Author(s): Shiva Kavosi
Air Force Research Lab
Abstract: We study dawn-dusk asymmetry in the occurrence rates of the Kelvin-Helmholtz instability at Earth’s magnetopause using data from the Time History of Events and Macroscale Interactions during Substorms (THEMIS) and Magnetospheric Multiscale (MMS) missions in conjunction with MHD modeling. The study revealed that the occurrence rates and locations of Kelvin-Helmholtz Waves (KHWs) exhibit a semiannual variation, peaking at the equinoxes and reaching a minimum at the solstice. Furthermore, these rates vary based on the polarity of the Interplanetary Magnetic Field (IMF) By, with a maximum occurrence observed around the fall equinox for negative IMF By and around the spring equinox for positive IMF By. The dawn-dusk and north-south asymmetry observed can be attributed to both the dipole tilt angle and the polarity of the IMF By; in the northern hemisphere, the Kelvin-Helmholtz instability favors the dawn sector for positive dipole tilt and the dusk sector for negative dipole tilt, and vice versa in the southern hemisphere. It is shown that asymmetry between dawn and dusk is controlled by both dipole and IMF By orientations.
Author(s): Léo Favier, Florent Miller, Philippe Laurent
LEPCHE – UMR AIM – CEA / Nucletudes; Nucletudes; LEPCHE – UMR AIM – CEA
Abstract: As part of the development of a compact radiation monitor, we developed a set of Monte Carlo simulations used to evaluate the response of a semi-conductor detector to cosmic-ray showers at ground level in order to help with experimental testing of the detector. The project specifically aims to calculate the response of the detector to the shower, the relative impact of albedo particles and the impact of the direct environment of the detector (i.e. the experiment room and bench) on the measurements.
So far, we use two simulation codes based on the Geant4 toolkit for the calculations. First, a large scale atmospheric shower code that injects high-energy cosmic-rays and solar particles in the exosphere and propagate them through a parametrised atmosphere towards the ground.
Depending on the model parameters, primary particles are first rigidity filtered, exposed to a bipolar magnetic field representing the Earth magnetosphere and then injected into the exosphere. Then, when reaching the lower parts of the thermosphere, the atmospheric model gets progressively more thinly resolved, down to the surface. Finally, the incident flux eventually generate albedo particles depending on the ground composition and humidity.
As an output, we are capable to establish both the prompt particle flux from the shower and the albedo flux emerging from the interaction between incident particle and the Earth’s surface.
The second code is a smaller scale representation of the detection device and its immediate environment, represented by a “typical laboratory environment”. Prompt and albedo spectra from the first simulation code are respectively injected by the top and the bottom of the simulation world, and are then propagated towards the detector. The code then outputs inward particle flux in the “lab” as well as energy deposition in the detector under the form of a library of spectra for all incident particle types and various physical configurations of the simulations.
In this poster, we will present these two simulations codes and some of the first results for the albedo and direct environment impact on the measured spectra, which will be key factors for the first experimental tests of our radiation monitor.
Author(s): Simeon Asenovski, Katya Georgieva, Boian Kirov
Space Research and Technology Institute – BAS; Space Research and Technology Institute – BAS; Space Research and Technology Institute – BAS
Abstract: This study investigates the long-term variability of the slow solar wind across the last five solar cycles and its impact on space weather. The slow solar wind, known for its complex and variable nature, influences Earth’s magnetosphere and, consequently, space weather conditions. By analyzing solar wind parameters and geomagnetic indices over multiple solar cycles, this research aims to identify patterns and trends in the behavior of the slow solar wind.
We utilize network modeling techniques to examine the relationships between solar wind variables and geomagnetic activity. This approach is intended to improve our understanding of the processes driving the variability of the slow solar wind and to enhance space weather forecasting models.
Author(s): Carlo Scotto, Dario Sabbagh, Alessandro Ippolito, Loredana Perrone
Istituto Nazionale di Geofisica e Vulcanologia; Istituto Nazionale di Geofisica e Vulcanologia; Istituto Nazionale di Geofisica e Vulcanologia; Istituto Nazionale di Geofisica e Vulcanologia
Abstract: Monthly median foF2 values derived from manual and automatic interpretations using ARTIST and Autoscala software over a 16-year period from 2006 to 2022. Data were analyzed for the hours between 23:00 and 00:00, employing two methods: one using exact hour data and another incorporating a quarter-hour before and after the hour. Statistical significance of the differences between automatic and manual values was determined using Student’s t-tests, with a p-value threshold of 0.05.
Results showed that both ARTIST and Autoscala demonstrated statistically significant differences in 14 out of 24 comparisons using exact hour data, with underestimation tendencies ranging from -0.037 to -0.117 for ARTIST and -0.003 to -0.109 for Autoscala. When data from a quarter-hour before and after the hour were included, significant differences were observed in 15 out of 24 comparisons for both systems, with ARTIST differences ranging from -0.035 to -0.08 and Autoscala from -0.036 to -0.08. Despite these statistically significant differences, many were within the measurement error margin of 0.1 MHz, suggesting a minimal practical impact.
The findings indicate that the median values obtained from ARTIST and Autoscala can reliably substitute manual interpretations for practical applications, given that the differences fall within acceptable error margins. This supports the adoption of automatic scaling tools for ionospheric data analysis, especially in observatories where manual scaling is impractical due to high labor costs and resource constraints.
Author(s): Giuseppina Carnevale, Mauro Regi, Patrizia Francia, Stefania Lepidi, Domenico Di Mauro
Istituto Nazionale di Geofisica e Vulcanologia, Italy; Istituto Nazionale di Geofisica e Vulcanologia, Italy; Università degli studi dell’Aquila, Italy; Istituto Nazionale di Geofisica e Vulcanologia, Italy; Istituto Nazionale di Geofisica e Vulcanologia, Italy
Abstract: We investigate the effects of Alfvénic and compressive fluctuations, typically present in corotating high-speed streams (HSS), on the geomagnetic activity at high latitudes in the low-frequency range (Pc5, 1-7 mHz), which is a range of frequency comparable to that of Alfvén waves in the Solar Wind (SW) at 1 AU. The study of Pc5 pulsations is important in the framework of space weather since they are responsible for the energization, transport, and precipitation of electrons in the radiation belts. We selected a corotating stream in the declining phase of solar cycle 23 and analyzed the corresponding geomagnetic field data at high-latitude geomagnetic observatories in both hemispheres.
For each observatory, we estimated a long-term geomagnetic power background in correspondence with quiet geomagnetic periods (low Kp index); then, we re-scaled the power to the background to better highlight the geomagnetic variations during the selected events. Regarding SW data, we rotated the interplanetary magnetic field (IMF) and SW velocity components at 1AU into the Mean ElectroMagnetic Field Aligned (MEMFA) reference frame to identify fluctuation along two main directions: one aligned and one orthogonal to the ambient magnetic field. We compared the rescaled geomagnetic field power with SW parameters, such as the power of IMF and SW velocity along the two directions, as well as with two quadratic invariants used to describe MHD turbulence: the normalized cross-helicity and the normalized residual energy. This combined method helps distinguish between compressive and Alfvénic fluctuations, providing insights into their impact on low-frequency geomagnetic variations.
Author(s): Kai Schennetten, Matthias M. Meier, Thomas Berger, Thomas Jahn, Daniel Matthiä, Mona C. Plettenberg, Markus Scheibinger, Michael Wirtz
Institute of Aerospace Medicine, German Aerospace Center (DLR); Institute of Aerospace Medicine, German Aerospace Center (DLR); Institute of Aerospace Medicine, German Aerospace Center (DLR); Lufthansa German Airlines; Institute of Aerospace Medicine, German Aerospace Center (DLR); Institute of Aerospace Medicine, German Aerospace Center (DLR); Lufthansa German Airlines; Institute of Aerospace Medicine, German Aerospace Center (DLR)
Abstract: The South Atlantic Anomaly (SAA) is a geographical region over the South Atlantic Ocean where the inner Van Allen radiation belt extends down particularly close to Earth. This leads to highly increased levels of ionizing radiation and related impacts on spacecraft in Low Earth Orbits, e.g., correspondingly increased radiation exposure of astronauts and electronic components on the International Space Station. According to an urban legend, the SAA is also supposed to affect the radiation field in the atmosphere even down to the altitudes of civil aviation. In order to identify and quantify any additional contributions to the omnipresent radiation exposure due to the Galactic Cosmic Radiation at flight altitudes, comprehensive measurements were performed crossing the geographical region of the SAA at an altitude of 13 km in a unique flight mission—Atlantic Kiss.
Author(s): Boian Kirov, Katya Georgieva, Simeon Asenovski
Space Research and Technology Institute at the Bulgarian Academy of Sciences; Space Research and Technology Institute at the Bulgarian Academy of Science; Space Research and Technology Institute at the Bulgarian Academy of Science
Abstract: The operation of space-based assets is increasingly threatened by various forms of space weather, which manifest in the form of satellite anomalies. These anomalies, which can lead to significant disruptions in satellite functionality, are primarily driven by solar phenomena such as Coronal Mass Ejections (CMEs), High-Speed Solar Winds (HSS), and Solar Proton Events (SPEs). This study presents a comprehensive analysis of the mechanisms by which these solar activities influence satellite anomalies, with a focus on the varying impacts across different orbital regimes, including Low Earth Orbit (LEO), Medium Earth Orbit (MEO), and Geostationary Earth Orbit (GEO).
Observations indicate that LEO satellites, due to their proximity to the Earth’s magnetosphere and Van Allen radiation belts, are particularly susceptible to Single Event Upsets (SEUs) caused by cosmic rays and trapped energetic ions. Meanwhile, GEO satellites are more prone to disruptions from SPEs and the cumulative effects of solar radiation. The study further examines the roles of deep-dielectric charging and surface charging—both absolute and differential—as significant contributors to satellite anomalies. The results demonstrate that these charging mechanisms can lead to various forms of discharges, including flashover between surfaces, punch-through from the interior to the surface, and discharges to space, each with distinct impacts on satellite subsystems.
The implications of these findings underscore the necessity of advancing our understanding of space weather interactions with satellite systems, as well as improving mitigation strategies, such as enhanced shielding, grounding techniques, and the use of radiation-hardened components. Future work will focus on refining predictive models to better anticipate satellite anomalies and minimize their operational impacts.
This study is supported by the National Science Fund of Bulgaria, Contract KP-06-N44/2 – 27-11-2020 “Space weather over a period of the century solar activity descending
OPS1-p23 Analyses of ionospheric and geomagnetic measurements during the April 8, 2024 solar eclipse
Author(s): Roberta Tozzi, Michael Pezzopane, Alessio Pignalberi, Igino Coco, Paola De Michelis, Fabio Giannattasio
Istituto Nazionale di Geofisica e Vulcanologia; Istituto Nazionale di Geofisica e Vulcanologia; Istituto Nazionale di Geofisica e Vulcanologia; Istituto Nazionale di Geofisica e Vulcanologia; Istituto Nazionale di Geofisica e Vulcanologia; Istituto Nazionale di Geofisica e Vulcanologia
Abstract: On April 8, 2024 a total solar eclipse occurred. The path of totality began in the South Pacific Ocean and, after crossing Mexico, the United States, and Canada, it ended in the Atlantic Ocean. Here, we report some analyses on ionospheric and geomagnetic ground-based and in-situ time series including the eclipse time window. A clear signature of the eclipse is well visible in the profilogram obtained from the ionograms recorded by the digisondes of Millstone Hill and Wallops Island, where the obscuration coverage exceeded 81%. Concerning the geomagnetic field, a set of 10 ground observatories affected by different percentages of obscuration is considered, with the aim of evaluating also the dependence of possible eclipse effects on the distance from the path of totality. Differently from digisonde data, geomagnetic data do not have an equally clear signature. Interestingly, one satellite of the ESA Swarm constellation crossed the eclipse path, so also in-situ electron density and temperature measurements have been included in the investigation. These show some anomalous patterns whose interpretation is however not univocal.
Author(s): Joseph Eggington
EDF R&D UK
Abstract: Space-Based Solar Power (SBSP) is a novel energy generation concept which involves harvesting solar energy in space via a kilometre scale spacecraft in a geostationary orbit (GEO). This energy is then converted to a microwave beam which is wirelessly transmitted to Earth and collected via a kilometre scale rectenna at a ground station. As these microwaves are mostly unaffected by the atmospheric conditions on Earth, SBSP overcomes many of the intermittency issues of terrestrial renewable energy, offering low-cost gigawatt levels of baseload energy generated continuously throughout the year. The concept is attracting an ever-growing volume of global research, with significant funding announced from a range of organisations including the European Space Agency. EDF R&D UK recently completed a UK Government-funded project “Space Based Energy Application Management (Space BEAM)”, which included the first detailed space weather risk analysis for an operational SBSP system.
Here we present results from this study, in which we assessed the potential impacts on the satellite, microwave beam, and ground-based system. This includes a probabilistic evaluation of the range of impacts over the system lifetime, based on estimates for space weather events over various return periods. We outline the relevant hazards along with a series of impact scenarios for events of varying magnitude, quantifying the potential impact on electricity costs. We find that if not properly mitigated through design and maintenance of the solar array, degradation from severe space weather could significantly reduce the system yield over time. Such events also pose a risk to the security and safe operation of the satellite and ground system. We make recommendations for future work which should carefully consider the risks from space weather to ensure resilient design and situational awareness during operation, along with appropriate mitigation strategies.
Author(s): Arpad Kis, István Lemperger, Veronika Barta, Kitti Berényi, Zoltán Vörös, Navin Kumar Dwivedi, Balázs Heilig, Gábor Hatos
HUN-REN Institute of Earth Physics and Space Science, 9400 Sopron, Csatkai E.-6-8, Hungary; 1HUN-REN Institute of Earth Physics and Space Science, 9400 Sopron, Csatkai E.-6-8, Hungary; 1HUN-REN Institute of Earth Physics and Space Science, 9400 Sopron, Csatkai E.-6-8, Hungary; 1HUN-REN Institute of Earth Physics and Space Science, 9400 Sopron, Csatkai E.-6-8, Hungary; 1HUN-REN Institute of Earth Physics and Space Science, 9400 Sopron, Csatkai E.-6-8, Hungary; 1HUN-REN Institute of Earth Physics and Space Science, 9400 Sopron, Csatkai E.-6-8, Hungary; 1HUN-REN Institute of Earth Physics and Space Science, 9400 Sopron, Csatkai E.-6-8, Hungary; 1HUN-REN Institute of Earth Physics and Space Science, 9400 Sopron, Csatkai E.-6-8, Hungary
Abstract: The space weather-related measurements at the Széchenyi István Geophysical Observatory (SzIGO), Hungary, have a long heritage: the magnetic and the telluric measurements were started in 1957. The Observatory was founded during the International Geophysical Year (in 1957-1958) as a dedicated research infrastructure of the electromagnetic (EM) phenomena of the solid Earth, upper atmosphere and near-Earth space. The observatory is situated on the southern shore of lake Fertő on thick conductive sediment within the Fertő-Hanság National Park. Its favorable situation shelters the observatory from most of the anthropogenic EM noises. On our poster, we present the latest developments in our measurement and data management system that can meet the modern needs of our times and is able to provide space weather related data in real-time and provide a warning service also.