Abstract Book of the Baltic Applied Astroinformatics and Space Data Processing (BAASP 2025) Conference

ABSTRACTS OF 9TH INTERNATIONAL SCIENTIFIC CONFERENCE “BALTIC APPLIED ASTROINFORMATICS AND SPACE DATA PROCESSING” 1 Abstracts of 9th International Scientific Conference “Baltic Applied Astroinformatics and Space Data Processing” (BAASP) November 12 - 13, 2025 Ventspils University of Applied Sciences https://en.venta.lv/baasp2025 DOI: 10.5281/zenodo.17552759 Editors: Vladislavs Bezrukovs & Ivars Šmelds & Aija Kalniņa 2025 2 The BAASP Conference Series serves as a platform for establishing and strengthening cross-border partnerships and knowledge exchange internationally in the Baltic region and globally. These conferences unite astronomers, space researchers and engineers, as well as experts in related disciplines including informatics, electronics, satellite technologies, geodesy, remote sensing, and environmental sciences. Conference Theme Space science is increasingly driven by the Big Data requiring robust data acquisition, management, processing, and interpretation capabilities. The interdisciplinary nature of astroinformatics combines space science with high-performance computing, AI, and machine learning, leading to breakthroughs in observational astronomy, satellite technologies, and Earthspace interactions. In recent years, Europe has continued to play an important role in next-generation astronomy. The continued expansion of the Low Frequency Array (LOFAR), antenna array telescope network across the continent, including the Baltic region, has enabled high-resolution studies of cosmic magnetism, solar activity, and transient radio phenomena. The European VLBI Network (EVN) has further enhanced its real-time e-VLBI capabilities and broadband sensitivity, with support from UK-based facilities such as Jodrell Bank and e-MERLIN. These advancements have contributed significantly to the precise localization of fast radio bursts and compact extragalactic sources. Technical developments also facilitate automated, rapid-response observation modes, which are essential to advancing multimessenger astronomy. This emerging field integrates radio, optical, gravitational wave, and neutrino data to probe energetic cosmic events such as neutron star mergers and magnetar outbursts. Concurrently, breakthroughs in AI-driven data mining, edge computing for satellite payloads, and quantum-enhanced algorithms are opening new frontiers in real-time analysis and autonomous decision-making for both Earth observation and deep-space missions. Meanwhile, the growing use of CubeSats and modular satellite platforms is reshaping the landscape of low-cost, high-impact space research, demanding new models for data integration, security, and interoperability across domains. BAASP 2025 will continue the dialogue on how emerging technologies transform astronomy, space science, geoscience, and remote observation. 3 CONTENTS Advances in Solar Radio Astronomy: Automation and Imaging with the RT-32 Telescope at Irbene 5 Aguirre E. Bezrukovs V., Bezrukovs D., Bouzarhoun El A. W., Janices I., Šteinberngs J., Orbidans A. Unraveling the Galactic Evolution of CNO: Precision Abundance Analysis Across Stellar Populations 6 Ambrosch M., Mikolaitis Š., Smiljanic R., Ernandes H., Drazdauskas A., Viscasillas-Vázquez C., Bale B., Ćurjurić B., Bagdonas V. Introducing the post-doctoral project: Revealing the physical mechanism of mass ejection around young massive stars via CH3OH masers 7 Aberfeldfs A. Microwave Observations of Coronal Holes at the 25th Solar Cycle 8 Bezrukovs D. Inspiring the next generation of students through active participation in radio astronomy research via international partnerships. 9 Bezrukovs V., Díaz S., Ruiz R., Yanguas P., Michalowski M., Kamiński K., Białobłocki P., Cazares J., Kalniņa A., Beltrán I., Blanco C., González L., Lagzdiņa I., Jakovicka S., Kowalewska K., Ziętara-Grzesiak W., Palacián J. F., Bosque R., Aranguren I. C. Multi-Epoch Radio Variability of BL Lacertae Observed with the Irbene Interferometer and MOJAVE Archival Data 10 Bezrukovs V., Burns R. A., Šteinbergs J., Šķirmante K., Aberfelds A., Shmeld I. Exploring VIRAC’s Capabilities for Radio Detection of Quasi-Periodic Pulsations in Solar and Stellar Coronae 11 Bezrukovs V., Burns R. A., Kolotkov D. Y., Nakariakov V. M., Šteinbergs J., Šķirmante K., Aberfelds A., Shmeld I., Bezrukovs D., Belov S.A., Kalniņa A. Variations in the radio continuum emission of high-mass protostars 12 Burns R. A., Aberfelds A., Shmeld I., Šteinbergs J., Šķirmante K., Bezrukovs V. Asteroid Observations from the Minor Planet Center Database: Opportunities and Challenges for Light Curve Analysis 13 Eglitis I., Nagainis K., Sokolova A. Temperatures of dust grains in some circumstellar environments 14 Freimanis J. Modeling Cosmogenic Isotopes as a Tool to Study Solar Energetic Events 15 Golubenko K., Rozanov E., Baroni M., Bard E., Sukhodolov T. Cometary activity modelling for ESA’s Comet Interceptor mission 16 Jasmonts G., Šķirmante K., Slavinskis A., Blumbergs K. Visualization Tools for Real-Time Near-Field RFI Monitoring at the LOFAR Station in Irbene 17 Janices I., Bezrukovs V., Šteinbergs J. The latest developments and patterns related to space debris issues. 18 Jotkus N. 4 Paths of formation for interstellar dense cloud cores 19 Kalvāns J. Structure and variability of astrophysical masers 20 Kalniņa A., Aberfelds A. Recent developments in Irbene antenna complex 21 Orbidāns A., Bleiders M., Bērziņš A., Laurinovičs R., Rasmanis R., et.al. Geomagnetic disturbances of the earth's magnetic field in the area of the Struve geodetic arc meridian 22 Orlyuk M., Romenets A., Marchenko A., Orliuk I. A Transformer-Based Forecasting Model for GNSS-VTEC and its Application Study Over Nigeria 23 Osatare A. W., Iluore C., Abiye B., Ozegin K. O. Solar eruptions near elongated regions of open magnetic fields 24 B.I. Ryabov., Vrublevskis A. On the programs of monitoring studies of space weather based on radio astronomical and magnetometric observations. 25 Ryabov M. I., Sukharev A.L., Usoskin I., Orlyuk M. I., Bezrukov V., Šteinbergs J., Romenets A.O., Zabora D.A. PauseMaker: Satellite communications with the mowing object 26 Šneps-Šneppe M. Preliminary results of observing ionosphere activity using 3C sources 27 Šteinbergs J., Mevius M., Shulevski A. MSCA Doctoral Network E-Sailors: Electric solar wind sail doctors 28 Slavinskis A. Ionospheric and magnetospheric responses to the 2025 solar eclipses 29 Sukharev A., Orlyuk M. I., Ryabov M. I., Usoskin, Kero A., Romenets A., Sumaruk Y., Kashuba V. I. , Bezrukovs V., Steinbergs J. Irradiation-Induced Structural Changes in Amino Acids: A Theoretical Study 30 Tamuliene J. Using Jupiter's Radio Storms to Probe the Solar Corona 31 Ulyanov O., Zarka P., Tiburzi C., Shevtsova A., Zakharenko V., Konovalenko O., Wucknitz O., Lamy L., . Grießmeier G-M., Skoryk M. , Kravtsov I., Bezrukovs V., Šteinbergs J., Skirmante K., Brazhenko A., Frantsuzenko A., Skoryk A. Millennium-scale solar eruptive events: Extreme space hazards 32 Usoskin I. Burst hub: get astronomical bursts together 33 Zheng S., Xiong S. Power-law Indices of EUV Intensity Power Spectrum in Flaring Coronal Active Regions 34 Zhong S., Kolotkov D. Y., Nakariakov V. M. 5 Advances in Solar Radio Astronomy: Automation and Imaging with the RT-32 Telescope at Irbene Aguirre E., Bezrukovs V., Bezrukovs D., Bouzarhoun E.A.W., Janices I., Šteinbergs J., Orbidans A. Aguirre Endika - Department of Electrical, Electronic and Communication Engineering of the Public University of Navarra (UPNA), Pamplona, Spain; [email protected] This work focuses on recent advancements in solar radio astronomy at the Ventspils International Radio Astronomy Centre (VIRAC), highlighting the modernization and automation of observational workflows using the RT-32 radio telescope. A comprehensive, full-stack web-based system has been developed and deployed to streamline solar observations at centimeter wavelengths. The primary goal of this system is to provide a secure, user-friendly environment that allows operators to manage the entire observational pipeline—from planning and scheduling to data acquisition and image generation—with minimal manual intervention. At the core of the platform is a powerful web interface that enables users to generate precise position files for solar tracking, schedule observation sessions, and monitor the status of ongoing work in real time. The system incorporates automated post-processing routines, including the creation, storage, and visualization of solar maps built from data collected via an antenna spiral scanning procedure. This raw data is processed using advanced image reconstruction techniques, such as bilinear interpolation and Gaussian filtering, which transform the raw observational samples into scientifically meaningful solar brightness maps. The entire infrastructure was built using open-source technologies and Python-based astronomical libraries. The result is a robust, scalable, and fully operational platform that significantly enhances the efficiency, reproducibility, and accessibility of solar radio observations. This solution marks a substantial step forward in modernizing the workflows of single-dish radio telescopes. 6 Unraveling the Galactic Evolution of CNO: Precision Abundance Analysis Across Stellar Populations Ambrosch M., Mikolaitis Š., Smiljanic R., Ernandes H., Drazdauskas A., Viscasillas-Vázquez C., Bale B., Ćurjurić B., Bagdonas V. Ambrosch Markus - Vilnius University, Institute of Theoretical Physics and Astronomy; [email protected] Carbon, nitrogen, and oxygen (CNO) are central to both stellar and Galactic chemical evolution, yet their enrichment history across the Milky Way is still not fully understood. This talk presents a project aimed at delivering a homogeneous and high-precision analysis of CNO abundances in a large and diverse sample of stars spanning all major Galactic components. Our strategy combines new spectroscopic observations with data from large stellar surveys, anchored by a set of well-characterized reference stars. This enables accurate calibration of stellar parameters and abundance measurements, along with precise age determinations (~10%) via isochrone fitting. By integrating chemical abundances, stellar ages, and orbital dynamics, we perform a population-level and radial migration analysis to trace the spatial and temporal evolution of CNO across the Galaxy. To fully exploit the rich datasets from modern surveys, we employ both classical physics-based spectroscopic methods and novel machine-learning techniques. This dual approach enhances the precision, consistency, and scalability of our analysis. Beyond Galactic enrichment, the project investigates the role of stellar mixing and magnetic activity in shaping surface abundances—an area still lacking robust observational constraints. These effects are crucial for understanding abundance patterns in evolved stars and improving stellar evolution models. 7 Introducing the post-doctoral project: Revealing the physical mechanism of mass ejection around young massive stars via CH3OH masers Aberfelds A. Aberfelds Artis - Engineering Research Institute Ventspils International Radio Astronomy Centre (ERI VIRAC) of Ventspils University of Applied Sciences (VUAS); [email protected] This project aims to shed light on the physical mechanism driving those striking outflows observed ubiquitously around young stars in our Galaxy. The large amount of gas and dust ejected away along the polar directions of a young star is generally referred to as an "outflow". Outflow phenomena are strictly related to the process of mass accretion into a star, regulating the time-scale of the accretion process and, in turn, the final stellar mass. Therefore, their understanding is fundamental to assessing our paradigm of star formation. Here, I propose to exploit the information coming from methanol maser emission, a unique tracer observed at the base of protostellar outflows, to systematically study, for the first time, how circumstellar gas is blown away at radii of a few 100 au (or less) from the star. Overall, this project is designed on a fine tuning between scientific objectives and instrumental facilities, with the aim to still enhance its impact with nextdecades observational facilities and to maximize my chances of becoming a major expert in the field. 8 Microwave Observations of Coronal Holes at the 25th Solar Cycle Bezrukovs D. Bezrukovs Dmitrijs - Engineering Research Institute Ventspils International Radio Astronomy Centre (ERI VIRAC) of Ventspils University of Applied Sciences (VUAS); [email protected] Studies of coronal holes and coronal hole-like areas with reduced brightness temperatures in microwaves have a significance to understand manifestations of the solar activity, distributions of plasma parameters in the solar corona and conditions of the creation of the solar wind and space weather. It's well known that the microwave emission of coronal holes has a low contrast to clearly observe and its visibility depends on the phase of the solar cycle and features of an instrument as well. The radio telescope RT-32 of Ventspils International Radio Astronomy Centre (VIRAC) provides routine 2D cartography of the polarized microwave emission of the Sun in wavelengths of 7.5-2.3 cm (4.1-14.2 GHz) with the low noise multichannel spectral polarimeter. Taking into account that the microwave emission is created at different heights into the corona spectral polarimetric observations offer the possibility to analyse the reduction of plasma densities and its distribution into coronal holes. The presentation concerns comparison of the microwave emission of some characteristic coronal holes observed with the radio telescope VIRAC RT-32 in 2019-2020 and 2024-2025 (the minimum and maximum of 25th solar cycle). Some attempts to evaluate the height distribution of plasma electron densities in the corona are presented also. 15 Modeling Cosmogenic Isotopes as a Tool to Study Solar Energetic Events Golubenko K., Rozanov E., Baroni M., Bard E., Sukhodolov T. Golubenko Kseniia - University of Oulu, Physics and Astronomy; [email protected] Understanding the long-term behaviour of the Sun is essential for both astrophysical research and assessing the potential impacts of extreme solar activity on Earth. Direct observations of solar energetic particles (SEPs) cover only the past few decades of the space age. To investigate stronger and rarer events over millennia, indirect evidence preserved in natural archives is required. One of the most powerful approaches relies on cosmogenic isotopes such as radiocarbon (14C) in tree rings, and beryllium-10 (10Be) and chlorine-36 in polar ice, which are produced in the atmosphere when cosmic rays or solar particles interact with nitrogen and oxygen nuclei. Numerical modeling of isotope production provides a link between measured concentrations in archives and solar processes. By combining physics-based simulations of particle transport in the atmosphere with carbon cycle and climate models (e.g. SOCOL model), it becomes possible to reconstruct the intensity and timing of past solar energetic particle events. This approach has revealed several extreme historical events that exceed anything observed during the instrumental era by orders of magnitude. We demonstrate how isotope modeling quantifies the magnitude and occurrence time of past solar particle storms, outline uncertainties related to atmospheric dynamics and data resolution, and place reconstructed events in the context of modern observations. Such reconstructions not only expand knowledge of solar variability but also help assess potential risks from extreme space weather to present-day technology. 16 Cometary activity modelling for ESA’s Comet Interceptor mission Jasmonts G., Šķirmante K., Slavinskis A., Blumbergs K. Jasmonts Gints - Engineering Research Institute Ventspils International Radio Astronomy Centre (ERI VIRAC) of Ventspils University of Applied Sciences (VUAS); [email protected] ESA’s Comet Interceptor will perform a rapid flyby of a dynamically new comet originating from the outer Solar System, potentially preserving materials that predate the Solar System itself. Because such objects follow highly eccentric orbits and are often discovered only a few months before perihelion, the mission will wait at the Sun-Earth L2 point until a suitable target is identified. This “unknown target” paradigm complicates pre-launch planning, since instrument development and calibration typically rely on well-characterized bodies. We address this challenge with physics-based models that span plausible comet activity states, including coma, transient outbursts, collimated jets, and resulting tail morphology. These models are embedded in a Blender based digital twin of the flyby, producing synthetic observations for MIRMIS, OPIC, and EnVisS across a range of phase angles, spin states, and activity levels. The environment enables assessment of data quality against instrument objectives as well as showcases unplanned scenarios of data acquisition. By leveraging the physically based Cycles rendering engine, we simulate light scattering of dust particles using phase functions and density fields derived from our models, yielding photometrically consistent imagery. We present representative scenarios, comparisons to previous observational data, and ongoing work to refine dust dynamics and photometric fidelity. This capability advances instrument readiness and operations planning when the real target remains unknown until late in the mission timeline. 17 Visualization Tools for Real-Time Near-Field RFI Monitoring at the LOFAR Station in Irbene Janices I., Bezrukovs V., Šteinbergs J. Janices Iñaki - Public University of Navarre Dpt. of Electrical, Electronic and Communications Engineering; ijanices[email protected] Radio Frequency Interference (RFI) remains a critical challenge in low-frequency radio astronomy, particularly for software-defined arrays like LOFAR (Low Frequency Array). This study presents a comprehensive approach to near-field RFI detection and visualization at the LOFAR station in Irbene, Latvia, operated by the Ventspils International Radio Astronomy Centre (VIRAC). Leveraging single-station interferometry and internal visibility data, we developed a modular imaging pipeline capable of generating near-field power maps across frequency, time, and height dimensions. The system integrates calibration routines, sweep-based imaging, and a real-time multithreaded processing engine with a web-based interface. This enables live monitoring of interference sources and supports field testing with controlled emitters. Field campaigns conducted at Irbene validated the system’s ability to detect and localize RFI sources with meter-level precision, even under constrained conditions. Key contributions include: • Adaptation of the open-source lofarimaging framework and use in near-field. • Implementation of sweep routines for dynamic RFI characterization. • Development of a real-time imaging and control interface with live tracking. • Deployment of a Docker-based environment for reproducibility and portability. This work improves LOFAR’s awareness of local interference and establishes a foundation for operational, station-level RFI monitoring tools. The system is publicly available via GitHub and supports future integration into broader diagnostic frameworks." 18 The latest developments and patterns related to space debris issues. Jotkus N. Jotkus Nansija - Engineering Research Institute Ventspils International Radio Astronomy Centre (ERI VIRAC) of Ventspils University of Applied Sciences (VUAS); [email protected] The issue of space debris is escalating due to an increasing number of satellite launches, ageing defunct satellites and fragments resulting from collisions and anti-satellite tests. Recent developments indicate technological and regulatory progress aimed at mitigating this risk, though significant challenges remain. The ESA has updated its Space Debris Mitigation Policy and Requirements (as of November 2023), shortening the disposal phase for Low Earth Orbit (LEO) objects from 25 years to 5 years, raising the success probability threshold for disposal operations and introducing interfaces to facilitate servicing or removal in the event of satellite failure. Meanwhile, the proposed EU Space Act (due to be introduced in mid-2025) seeks to standardise regulations across Member States, ensuring the safety, resilience and environmental sustainability of space operations. This includes the introduction of stricter rules for debris tracking and mitigation. There is also increasing industry cooperation: the ESA's “Zero Debris Charter” encourages entities to commit to preventing new debris, and dialogues are taking place (e.g. with commercial operators) about joining these voluntary charters. 19 Paths of formation for interstellar dense cloud cores Kalvāns J. Kalvāns Juris - Engineering Research Institute Ventspils International Radio Astronomy Centre (ERI VIRAC) of Ventspils University of Applied Sciences (VUAS); [email protected] The starless cores of interstellar clouds are a standard case for simple astrochemical modelling, often used to test new methods and theories. The physical formation of such dense cores is regulated by large-scale processes and cannot be described by an isolated evolution scenario of the core itself. We describe several paths how evolving physical conditions arrive at those characteristic for dense cores. The validity of each scenario is tested with an astrochemical model by comparing calculated abundances of interstellar ice species to observations. Five central density evolution paths were considered: exponential, linear, sigmoid (S-type), and asymptotic growth, as well as gravitational infall. Two time-scales – 1 Myr and 3 Myr – were applied for each case. Increase of the central density was accompanied by contraction of a spherical (1D) molecular cloud with a constant mass. Results. The exponential, infall, linear, and sigmoid density evolution scenarios are apparently all able to replicate observed ice composition, each with its own time-scale. Additional chemical evolution in long-lived cores with steady conditions is essential for explaining disagreements in ice abundances. The results indicate a consistent 0.5 Myr-long active growth stage for dense cloud cores, in addition to periods of slower contraction before or after the active stage. Finally, we find that the often-used simple models starting with atomic chemical composition in dense core conditions produce ice species' abundances that are incompatible with observations. 20 Structure and variability of astrophysical masers Kalniņa A., Aberfelds A. Kalniņa Aija - Engineering Research Institute Ventspils International Radio Astronomy Centre (ERI VIRAC) of Ventspils University of Applied Sciences (VUAS); [email protected] We observed 2 methanol maser sources G32.03+0.06, G35.20 -1.74 (W48) at 6.7 GHz using the European VLBI Network (EVN). These masers have been systematically monitored over the past five years with the Irbene 16 m and 32 m radio telescopes [1]. Selected sources have different variability types periodic, quasi-periodic, long-term dimming. Our primary objectives are to investigate the proper motions, variability mechanisms, source morphology, and cloudlet structure evolution of these masers. We aim to identify the physical processes driving maser variability and improve our understanding of the underlying astrophysical conditions. [1] A. Aberfelds, J. Šteinbergs, I. Shmeld, R. A. Burns, ‘’Five years of 6.7-GHz methanol maser monitoring with Irbene radio telescopes” Monthly Notices of the Royal Astronomical Society,Volume 526, Issue 4, December 2023, Pages 5699–5714, https://doi.org/10.1093/mnras/stad3158 21 Recent developments in Irbene antenna complex Orbidāns A., Bleiders M., Bērziņš A., Laurinovičs R., Rasmanis R., et.al. Orbidāns Artūrs - Engineering Research Institute Ventspils International Radio Astronomy Centre (ERI VIRAC) of Ventspils University of Applied Sciences (VUAS); [email protected] During the last few years, multiple projects have been carried out to continuously upgrade the receiving capabilities of the Irbene antennas RT-32 and RT-16, as well as to establish transmitting capabilities for both antennas. Development of new feed horns, RF networks, receivers, and cryostats etc. has been undertaken with the goal of enabling deep-space communications, with special emphasis on future Lunar missions. In parallel, the needs of radio astronomy are being addressed through the development of new cryogenic L/S-band receiver and by supporting various international scientific projects. These improvements significantly enhance the overall sensitivity and operational flexibility of the Irbene antenna complex, positioning it as a key infrastructure for both scientific research and space mission support. During this talk, the audience will be introduced to the current technical capabilities of the Irbene antennas, recent development achievements, and future plans for expanding their role in deep-space and radio astronomical research. 22 Geomagnetic disturbances of the earth's magnetic field in the area of the Struve geodetic arc meridian Orlyuk M., Romenets A., Marchenko A., Orliuk I. Orlyuk Mykhailo - Subbotin Institute of Geophysics of the National Academy of Sciences of Ukraine; [email protected]t At present, the issues of solar-terrestrial interactions are very relevant, especially the mechanisms of transmission of deep space disturbances to the Earth's surface. One of the main components of the solar-terrestrial interactions is the magnetic field. It, on the one hand, serves as a link between the Sun and the Earth, and, on the other hand, causes a different response to the same impact depending on the “relief” of the Earth's internal magnetic field. To do this, we investigated the “reaction” of the Earth's magnetic field to the coronal mass ejection of May 7, 2024, which reached the Earth's orbit on May 10, 2024, and the associated magnetic storm that lasted more than 24 hours. The influence of high-energy sources of external origin on magnetospheric-ionospheric processes and related perturbations of the Earth's outer and inner shells is well understood. The interaction of the magnetospheric-ionospheric geomagnetic disturbance with the Earth's internal magnetic field remains less studied. In this regard, we studied the perturbations of the Earth's magnetic field along the meridian Struve Geodetic Arc (SGA). The SGA meridian is characterized by significant changes in the Earth's main magnetic field (core field) and anomalous magnetic field (lithosphere field). There are 7 magnetic observatories in the vicinity of the SGA, which makes it possible to assess the nature of magnetic storm on May 10-13, 2024, depending on the global and regional characteristics of the Earth's internal magnetic field. 23 A Transformer-Based Forecasting Model for GNSS-VTEC and its Application Study Over Nigeria Osatare A. W., Iluore C., Abiye B., Ozegin K. O. Osatare Aghedo Williams - University of Nigeria, Department of Physics and Astronomy, Nsukka 400241, Nigeria; [email protected] This paper presents a novel approach using channel-independent patch time series Transformer (PatchTST) for GPS-VTEC forecasting. This is the first time that a Patch Time Series Transformer (PatchTST) framework has been integrated into GPS-VTEC forecasting, demonstrating its applicability to ionospheric prediction. We construct the GPS-VTEC dataset using observations from Nigeria, leveraging data collected from ionospheric monitoring stations. Factors influencing GPS-VTEC variations, such as seasonal changes, diurnal patterns, magnetic activity, and solar activity, are identified and incorporated as input parameters for the models. Training is conducted using data from the year 2012–2021, while the model performance is evaluated using the year 2022 data, a period of high solar activity. We compare the performance of PatchTST, MLP, LSTM, BiGRU, and CNNBiGRU models, evaluating their forecasting accuracy using root mean squared error (RMSE), mean absolute percentage error (MAPE), and correlation coefficient (R). The PatchTST model achieves an RMSE of 4.731 TECU, a MAPE of 2.351%, and an R-value of 0.986, outperforming traditional deep learning models in short-term (1-day) and mid-term forecasting. The hybrid CNNBiGRU model also shows strong predictive capability, achieving an RMSE of 3.046 TECU and an R-value of 0.896, effectively capturing diurnal variations of GPS-VTEC. Additionally, uncertainty analysis reveals that PatchTST exhibits superior adaptability to model uncertainty, showing a 62.9% improvement in mean error (ME) and a 40.5% improvement in standard mean error (STDE) compared to benchmark models. Comparisons with IRI-2016 and NeQuick-2 models indicate that while PatchTST provides more accurate predictions than all the models including the deep learning models and the empirical models in capturing seasonal variations across the dataset. 24 Solar eruptions near elongated regions of open magnetic fields Ryabov. B.I., Vrublevskis A. Ryabov Boriss - Engineering Research Institute Ventspils International Radio Astronomy Centre (ERI VIRAC) of Ventspils University of Applied Sciences (VUAS); [email protected] Solar flares and coronal mass ejections (CMEs) are the most powerful phenomena on the Sun believed to be caused by instabilities in solar magnetic fields. We examine how narrow elongated regions of open magnetic fields relate to these phenomena. For this purpose CMEs and the associated solar flares are traced near an elongated open-field region during January - March 2013. By modelling coronal fields with the Potential Field Source Surface model (PFSS), we reveal high squashing of field lines. Since such high squashing promotes reconnection of magnetic field lines, we recognize there the potential for triggering the eruptions. A set of extreme ultraviolet images from the AIA instrument on board the Solar Dynamic Observatory also implies long-lasting (up to 5 - 10 hours) events of magnetic reconnection in the post-flare arcade and the coronal dimming accompanying a CME. We conclude that by enabling sustained field line reconnection the narrow regions of open-fields are possibly linked to the nearby solar eruptions. This research is funded by the European Regional Development Fund, project "ERA Chair in Astrophysics, 350 Instrumentation, Ground Segment Technologies and Space Photonics at the University of Latvia", project No. 351 1.1.1.5/2/24/A/004. 31 Using Jupiter's Radio Storms to Probe the Solar Corona Ulyanov O., Zarka P., Tiburzi C., Shevtsova A., Zakharenko V., Konovalenko O., Wucknitz O., Lamy L., Grießmeier G-M., Skoryk M., Kravtsov I., Bezrukovs V., Šteinbergs J., Skirmante K., Brazhenko A., Frantsuzenko A., Skoryk A. Ulyanov Oleg - Institute of Radio Astronomy, National Academy of Sciences of Ukraine, Kharkiv, 61002 Ukraine; oulya[email protected] Low-frequency observations of various types of bursts generated in the solar corona have one common feature. In the decameter-meter ranges, they all have predominantly one circular polarization. This polarization is associated with the normal mode of that ordinary/extraordinary wave, which has a lower attenuation coefficient. One possible explanation for these polarization characteristics of low-frequency solar bursts is that they originate at relatively high altitudes (1.52 Rsun), where the intensity of the magnetic field in the solar corona is ~ 1G. Furthermore, propagating towards Earth, one of these waves attenuates more than the other due to greater interaction with the Sun's magnetic field and, accordingly, greater optical thickness. However, this explanation is incomplete, as it does not explain how magnetic fields with low intensities keep subrelativistic electron beams, which generate various types of bursts, from Coulomb repulsion. On the other hand, the circular polarization may be imposed by the moving electrons themselves over large sections of the coronal magnetic field, in which case the polarization of solar bursts is determined by the electron’s motion. For a more detailed study of the corona plasma properties, observations of Jupiter's eclipse by the Sun's corona were carried out. These observations were carried out from May to August 2025. In this case, decameter radio storms, which occurred episodically in the Jupiter-Io tube, were considered by us as a point broadband pulsed source of elliptically polarized radiation. This radio emission was used to probe the Sun's corona at various elongations. In particular, we managed to record a Jupiter radio storm 2 degrees from the Sun center. To determine the parameters of the solar corona plasma, we will study such propagation effects as scattering and dynamic rotation measure, which will allow us to estimate the parameters of magnetized plasma in the Sun's corona. 32 Millennium-scale solar eruptive events: Extreme space hazards Usoskin I. Usoskin Ilya - University of Oulu, Sodankylä geophysical Observatory; ilya.uso[email protected] The Sun is a variable star, sometimes producing eruptive events such as flares and coronal mass ejections, which can disrupt the near-Earth environment and pose significant threats to modern technological society. As discovered recently using indirect proxy data, the Sun can rarely produce extreme solar particle events (ESPEs). Presently, seven events and two candidates are known for the past 14 millennia, making them millennium-scale events. ESPEs can be orders of magnitude stronger than the strongest events directly observed during the last decades. A summary of the current knowledge of the occurrence rates and reconstructed parameters of the ESPEs is discussed in the context of the possible terrestrial effects, such as radiation dose and regional climate. 33 Burst hub: get astronomical bursts together Zheng S., Xiong S. Zheng Shijie - Institute of High Energy Physics, CAS, Particle Astrophysics Center; [email protected] In the era of multi-messenger multi wavelength astronomy, it is of critical importance to make joint observations with various telescopes and instruments in a timely manner. These observations usually will be reported as various types of Messages in different platforms, which is somewhat inconvenient for researchers. We collect these Messages from various platform and group them into astronomical burst Events with AI and provide statistics of all and the latest Events and Messages and highlight the most popular Events (called Hot Events). 34 Power-law Indices of EUV Intensity Power Spectrum in Flaring Coronal Active Regions Zhong S., Kolotkov D. Y., Nakariakov V. M. Zhong Sihui - KU Leuven, Department of Mathematics; [email protected] Solar intensity power spectra are usually characterised by coloured noise, with the spectral energy following a segmented power-law function of frequency, S(f) ∝ f⁻ᵅ over different frequency ranges. Typically, the power-law index exceeds 1 in the low-frequency part (αₗf) and is around 0 at high frequencies (αₕf). This work investigates the spatial and temporal evolution of the power-law indices of coronal EUV intensity power spectra in flare-hosting active regions. The spatial distribution of the power-law index in the low-frequency domain (αₗf) closely mirrors EUV intensity images, indicating that αₗ can reveal the dynamics of coronal plasma structures. Temporally, αₗf remains stable in quiescent active regions, but it exhibits significant variability before the flare onset. Motivated by this behaviour, we analysed 14 flare events, quantifying the temporal variation of the indices αₗf and αₕf as potential flare precursors. In all flare events considered, notable deviations of αₗf beyond a defined threshold consistently occurred at the flare site within a few minutes before the flare. In some cases, the change in the value of αₗf − αₕf was detected within 30–90 minutes before the flare. These findings suggest that the temporal variation of the power-law indices in coronal EUV intensity power spectra could potentially serve as shortterm precursors of solar flares, which needs to be validated on a larger flare sample. 35