{"id":248,"date":"2019-09-18T10:34:32","date_gmt":"2019-09-18T08:34:32","guid":{"rendered":"https:\/\/ibws.cz\/?page_id=248"},"modified":"2025-04-22T15:48:30","modified_gmt":"2025-04-22T13:48:30","slug":"list-of-abstracts","status":"publish","type":"page","link":"https:\/\/ibws.cz\/index.php\/conference\/list-of-abstracts\/","title":{"rendered":"List of Abstracts"},"content":{"rendered":"<p>[et_pb_section fb_built=&#8221;1&#8243; next_background_color=&#8221;#091744&#8243; disabled_on=&#8221;off|off|off&#8221; admin_label=&#8221;Header&#8221; _builder_version=&#8221;4.16&#8243; background_color=&#8221;#091744&#8243; use_background_color_gradient=&#8221;on&#8221; background_color_gradient_stops=&#8221;#091744 0%|#091744 100%&#8221; background_color_gradient_start=&#8221;#091744&#8243; background_color_gradient_end=&#8221;#091744&#8243; background_image=&#8221;https:\/\/ibws.cz\/wp-content\/uploads\/2019\/11\/gaming-04.jpg&#8221; parallax=&#8221;on&#8221; custom_margin=&#8221;||-49px|||&#8221; custom_padding=&#8221;8vw||7vw||false|false&#8221; bottom_divider_style=&#8221;ramp2&#8243; bottom_divider_height=&#8221;24vw&#8221; bottom_divider_flip=&#8221;horizontal&#8221; global_colors_info=&#8221;{}&#8221;][et_pb_row _builder_version=&#8221;4.16&#8243; global_colors_info=&#8221;{}&#8221;][et_pb_column type=&#8221;4_4&#8243; _builder_version=&#8221;4.16&#8243; custom_padding=&#8221;|||&#8221; global_colors_info=&#8221;{}&#8221; custom_padding__hover=&#8221;|||&#8221;][et_pb_image src=&#8221;https:\/\/ibws.cz\/wp-content\/uploads\/2019\/11\/gaming-05.png&#8221; align=&#8221;center&#8221; align_tablet=&#8221;center&#8221; align_phone=&#8221;&#8221; align_last_edited=&#8221;on|desktop&#8221; _builder_version=&#8221;4.16&#8243; animation_style=&#8221;roll&#8221; animation_duration=&#8221;3000ms&#8221; animation_intensity_roll=&#8221;3%&#8221; animation_starting_opacity=&#8221;100%&#8221; global_colors_info=&#8221;{}&#8221;][\/et_pb_image][et_pb_text _builder_version=&#8221;4.16&#8243; text_font=&#8221;Lato||||||||&#8221; text_font_size=&#8221;16px&#8221; text_line_height=&#8221;2em&#8221; header_font=&#8221;Rubik|700||on|||||&#8221; header_font_size=&#8221;70px&#8221; header_line_height=&#8221;1.2em&#8221; text_orientation=&#8221;center&#8221; background_layout=&#8221;dark&#8221; header_font_size_tablet=&#8221;50px&#8221; header_font_size_phone=&#8221;40px&#8221; header_font_size_last_edited=&#8221;on|phone&#8221; global_colors_info=&#8221;{}&#8221;]<\/p>\n<h1>List of abstracts<br \/> 2026<\/h1>\n<p>[\/et_pb_text][\/et_pb_column][\/et_pb_row][et_pb_row column_structure=&#8221;1_3,1_3,1_3&#8243; disabled_on=&#8221;off|off|off&#8221; _builder_version=&#8221;4.16&#8243; global_colors_info=&#8221;{}&#8221;][et_pb_column type=&#8221;1_3&#8243; _builder_version=&#8221;4.16&#8243; custom_padding=&#8221;|||&#8221; global_colors_info=&#8221;{}&#8221; custom_padding__hover=&#8221;|||&#8221;][et_pb_button button_url=&#8221;#HEA&#8221; button_text=&#8221;HEA&#8221; button_alignment=&#8221;center&#8221; 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box_shadow_color__hover_enabled=&#8221;rgba(0,0,0,0.3)&#8221; sticky_enabled=&#8221;0&#8243;][\/et_pb_button][\/et_pb_column][et_pb_column type=&#8221;1_3&#8243; _builder_version=&#8221;4.16&#8243; custom_padding=&#8221;|||&#8221; global_colors_info=&#8221;{}&#8221; custom_padding__hover=&#8221;|||&#8221;][et_pb_button button_url=&#8221;#SAT&#8221; button_text=&#8221;SAT&#8221; button_alignment=&#8221;center&#8221; _builder_version=&#8221;4.23.4&#8243; custom_button=&#8221;on&#8221; button_text_size=&#8221;14px&#8221; button_text_color=&#8221;#ffffff&#8221; button_bg_color=&#8221;#1f3065&#8243; button_border_width=&#8221;0px&#8221; button_border_radius=&#8221;100px&#8221; button_letter_spacing=&#8221;1px&#8221; button_font=&#8221;Rubik|500||on|||||&#8221; custom_padding=&#8221;10px|60px|10px|60px|true|true&#8221; hover_enabled=&#8221;0&#8243; button_letter_spacing_last_edited=&#8221;off|desktop&#8221; locked=&#8221;off&#8221; global_colors_info=&#8221;{}&#8221; button_letter_spacing__hover=&#8221;3px&#8221; 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disabled_on=&#8221;on|on|off&#8221; _builder_version=&#8221;4.16&#8243; use_background_color_gradient=&#8221;on&#8221; background_color_gradient_direction=&#8221;210deg&#8221; background_color_gradient_stops=&#8221;#1a448b 0%|#00b0db 100%&#8221; background_color_gradient_start=&#8221;#1a448b&#8221; background_color_gradient_end=&#8221;#00b0db&#8221; transform_scale=&#8221;105%|105%&#8221; z_index=&#8221;2&#8243; width=&#8221;300px&#8221; width_tablet=&#8221;&#8221; width_phone=&#8221;200px&#8221; width_last_edited=&#8221;on|desktop&#8221; max_width=&#8221;10%&#8221; module_alignment=&#8221;right&#8221; custom_margin=&#8221;|auto||869px|false|false&#8221; custom_padding=&#8221;1%|1%|3%|1%|false|false&#8221; custom_padding_tablet=&#8221;|10vw||10vw||true&#8221; custom_padding_phone=&#8221;60px||||false&#8221; animation_style=&#8221;fold&#8221; animation_direction=&#8221;right&#8221; animation_intensity_fold=&#8221;20%&#8221; background_color_gradient_stops_tablet=&#8221;#1a448b 0%|#00b0db 100%&#8221; 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_builder_version=&#8221;4.16&#8243; background_color=&#8221;#091744&#8243; background_image=&#8221;https:\/\/ibws.cz\/wp-content\/uploads\/2019\/11\/gaming-22.png&#8221; background_size=&#8221;initial&#8221; background_repeat=&#8221;repeat&#8221; min_height=&#8221;25vh&#8221; custom_padding=&#8221;0px||0px||false|false&#8221; bottom_divider_style=&#8221;ramp2&#8243; bottom_divider_color=&#8221;#091744&#8243; bottom_divider_height=&#8221;14vw&#8221; global_colors_info=&#8221;{}&#8221; box_shadow_style__hover=&#8221;none&#8221; box_shadow_style__hover_enabled=&#8221;none&#8221; box_shadow_color__hover=&#8221;rgba(0,0,0,0.3)&#8221; box_shadow_color__hover_enabled=&#8221;rgba(0,0,0,0.3)&#8221;][et_pb_row _builder_version=&#8221;4.16&#8243; global_colors_info=&#8221;{}&#8221;][et_pb_column type=&#8221;4_4&#8243; _builder_version=&#8221;4.16&#8243; global_colors_info=&#8221;{}&#8221;][et_pb_text _builder_version=&#8221;4.16&#8243; global_colors_info=&#8221;{}&#8221;]<\/p>\n<link rel=\"stylesheet\" href=\"https:\/\/fonts.googleapis.com\/icon?family=Material+Icons\"><h2 style='color: var(--conf-color-abstract-session);' id=\"HEA\">High Energy Astrophysics<span style='font-size: 18px; vertical-align: text-bottom; margin-left:20px;'> <i class=\"material-icons\" style=\"vertical-align: middle;\">record_voice_over<\/i> 10<\/span><\/h2><div style=\"margin-left: 20px\"><i class=\"material-icons\" style='vertical-align: text-bottom'>record_voice_over<\/i> <b><span class=\"name\">Tristan Bouchet <\/span><\/b><br><span class=\"title\">Spectro-polarization with INTEGRAL: application to Cygnus X-1<\/span><br><p class=\"abstract\">In this new era of high-energy spectro-polarimetry, our understanding of high-energy sources has the potential to be greatly improved. This is especially the case for Black Hole X-ray Binaries (BHXB), also known as Microquasars, for which many unresolved challenges remain. In particular acceleration mechanisms and how they relate to accretion-ejection processes. Combined with spectroscopy, polarization is a powerful tool to reveal the geometry of the system and the configuration of the magnetic fields.\r\n\r\nThe persistent Microquasar Cygnus X-1 is particularly well suited for our analysis. In soft X-rays, the polarization is low and aligned with the general direction of the jet, while the polarization angle in the soft gamma-rays is found close to 70\u00b0 away from the jet. We use a novel method to combine high-energy spectra and polarization of this bright source from 1 keV to 2 MeV in a single fit, including observations from IXPE, PoGO+, XL-Calibur, AstroSat, INTEGRAL\/SPI and INTEGRAL\/IBIS. Our study involves energy-dependent polarization models for both emission processes, in part inspired by similar studies on Blazars.\r\n\r\nPreliminary results already reveal new constraints about the non-thermal hard-tail origin (above 100 keV), in particular its high-energy spectral cut-off and the degree of order of the magnetic field.<\/p><\/div><br><div style=\"margin-left: 20px\"><i class=\"material-icons\" style='vertical-align: text-bottom'>record_voice_over<\/i> <b><span class=\"name\">Rene Hudec <\/span><\/b><br><span class=\"title\">IBWS Introduction and Historical Backgroundf<\/span><br><p class=\"abstract\">Originally, the IBWS (INTEGRAL\/BART) workshops focused on the work of High energy\r\nastrophysics group (at that dime dominated by young research fellows and students) in\r\nAstronomical Institute of the Academy of Sciences of the Czech Republic and relevant\r\nnational and international collaborators from the field, with intensive student participation.\r\nDuring the early years, these activities were focussed on the ESA INTEGRAL satellite and\r\non the related ground-based robotic telescopes, e.g. the small robotic BART telescope\r\nat the Ondrejov Observatory.\r\nNowadays, the IBWS workshops promote regional collaboration in galactic and\r\nextragalactic high-energy astrophysics, both experimental as well as theoretical, with an\r\nemphasis on the interface between satellite projects and ground-based experiments (e.g.\r\nrobotic telescopes). We continue our emphasis on wide participation and presentations of\r\nstudents and young research fellows.<\/p><\/div><br><div style=\"margin-left: 20px\"><i class=\"material-icons\" style='vertical-align: text-bottom'>record_voice_over<\/i> <b><span class=\"name\">Bendeg\u00faz Koncz <\/span><\/b><br><span class=\"title\">Galaxy mergers history in the IllustrisTNG simulation<\/span><br><p class=\"abstract\">Galaxy evolution over time remains unclear, with ongoing debate about how collisions affect star formation and metallicity. The role of the local environment shaped by the large-scale structure of the Universe in galaxy mergers may be significant, yet it has not been thoroughly examined. Using the IllustrisTNG cosmological simulation, we processed the catalog data and merger tree files of the TNG300-1 run. We calculated the average star formation rate (SFR) and stellar mass of galaxies over the redshift range 0 < z < 15 to trace the cosmic star formation history and galaxy growth. We investigated the environments of galaxy mergers with a focus on local density within the cosmic web, and found that interactions with gas-rich dwarf galaxies can trigger a resurgence in gas supply, highlighting the importance of gas dynamics in sustaining star formation. We compared our results with recent JWST observations and identified differences in the star formation rate density (SFRD) history between simulations and observations, providing new insights into early galaxy formation and evolution. See Koncz et. al. Universe 2025, 11(9), 286.<\/p><\/div><br><div style=\"margin-left: 20px\"><i class=\"material-icons\" style='vertical-align: text-bottom'>record_voice_over<\/i> <b><span class=\"name\">Saurabh Mittal <\/span><\/b><br><span class=\"title\">Contribution of Stellar flares to the 511 keV Galactic positron budget<\/span><br><p class=\"abstract\">The origin of the Galactic 511 keV positron annihilation line has been a mystery for five decades. One proposed explanation is positron production in stellar flares, motivated by the detection of the 511 keV line in solar flares and by the association of this emission with old stellar populations. In this work, we explore this scenario using two complementary approaches. First, we build a theoretical model to estimate the quasi-persistent 511 keV emission from flaring stars. Starting from solar flare observations, we construct empirical scaling relations between flare energy and 511 keV luminosity and extend them to Galactic stellar populations using flare-frequency-energy distributions for different spectral types. In parallel, we analyze INTEGRAL\/SPI data in the 511 keV band using combinations of known point sources and simple spatial templates, such as disk and bulge components modeled as two-dimensional Gaussians. We also test alternative descriptions in which no bulge template is assumed and the emission is instead described by a disk component together with a population of globular clusters, scaled by their masses and distances. This ongoing work aims to assess whether stellar flares can plausibly account for the observed Galactic 511 keV emission.<\/p><\/div><br><div style=\"margin-left: 20px\"><i class=\"material-icons\" style='vertical-align: text-bottom'>record_voice_over<\/i> <b><span class=\"name\">Ondrej Pejcha <\/span><\/b><br><span class=\"title\">Evolution of binary stars leading up to high-energy sources<\/span><br><p class=\"abstract\">Many stellar high-energy sources are manifestations of one of the stages of binary star evolution. In this talk, I will discuss the astrophysical processes influencing binary star evolution such as mass transfer and the response of mass-losing and mass-accreting stars, formation of circumbinary medium, explosions, and violent events such as common envelope evolution, as well as their relation to end products such as gravitational wave sources. I will cover in greater detail two types of transient events: luminous red novae, which accompany stellar mergers and potentially hold the key to connecting many different evolutionary pathways , and classical novae, where recent GeV Fermi detections as well as ground, space, and interferometric observations suggest a much more complicated picture of mass ejection than previously thought.<\/p><\/div><br><div style=\"margin-left: 20px\"><i class=\"material-icons\" style='vertical-align: text-bottom'>record_voice_over<\/i> <b><span class=\"name\">Thomas Siegert <\/span><\/b><br><span class=\"title\">Nuclear Astrophysics and Gamma-Rays:\u2028From Space to Earth<\/span><br><p class=\"abstract\">Gamma rays provide a unique window on nuclear processes occurring throughout the Universe, directly tracing radioactive isotopes and matter antimatter annihilation.\r\nIn this talk, I will review key results from gamma-ray line spectroscopy in space, focusing on observations from 22 years of the now completed ESA satellite mission INTEGRAL. Measurements of radioactive isotopes, such as 26Al and 60Fe, reveal ongoing nucleosynthesis in the Galaxy and connect stellar explosions to traces found on Earth, including signatures preserved in ocean crust sediments. In this context, the long-standing puzzle of the Galactic 511 keV positron annihilation emission is also discussed.\r\nNASA\u2019s Compton Spectrometer and Imager (COSI) mission, scheduled for launch in 2027, is expected to significantly advance MeV measurements thanks to its increased sensitivity and imaging capabilities. I will introduce the Compton telescope concept and highlight open questions addressed by COSI, such as the role of massive stars and supernovae in Galactic feedback.\r\nFinally, I will show how analysis and imaging techniques developed for space-based gamma-ray astronomy are now being applied on Earth, enabling isotopic imaging of radioactive residues in nuclear facilities and related environments.<\/p><\/div><br><div style=\"margin-left: 20px\"><i class=\"material-icons\" style='vertical-align: text-bottom'>record_voice_over<\/i> <b><span class=\"name\">N\u00f3ra Varga <\/span><\/b><br><span class=\"title\">The Potential of the THESEUS Mission for Studies of Young Stellar Objects<\/span><br><p class=\"abstract\">The Transient High-Energy Sky and Early Universe Surveyor (THESEUS) is a space mission concept designed to perform repeated wide-area surveys of the sky, primarily to detect and characterize high-redshift gamma-ray bursts. As a consequence of its baseline observing strategy, THESEUS will also provide systematic, time-dependent coverage of large fractions of the sky in the soft X-ray and near-infrared domains, offering new opportunities for studies of Galactic sources beyond its core cosmological goals.\r\nWe aim to assess the observability of nearby star-forming regions and young stellar objects (YSOs) within the baseline survey strategy of THESEUS. We investigate how the mission\u2019s pointing concept and sky-coverage pattern translate into the temporal visibility of prominent nearby star-forming complexes and how this visibility is distributed over the mission lifetime. <\/p><\/div><br><div style=\"margin-left: 20px\"><i class=\"material-icons\" style='vertical-align: text-bottom'>record_voice_over<\/i> <b><span class=\"name\">Tauseef Ahmad Zafar <\/span><\/b><br><span class=\"title\">Data mining in astronomical photographic archives with advanced IT methods<\/span><br><p class=\"abstract\">We report on recent progress in the digitization of astronomical plate archives and the application of novel IT approaches, including machine learning methods, to these data. Astronomical photographic archives represent an extensive and largely untapped database of stellar, solar, and planetary observations, encompassing astrometric, photometric, and spectroscopic measurements accumulated over more than a century. These archives hold significant potential for a wide range of applications in modern astrophysics, including the study of long-term variability, detection of rare transient events, and identification of objects with peculiar spectra. We present results from visits to over 16 US institutions and numerous European, Mexican, and Chinese observatories, where plate samples were digitized using a transportable scanning device. We further describe the application of advanced computational techniques to digitized plates from the Sonneberg Observatory and the Henize Mt. Wilson Michigan Southern Sky Survey, demonstrating the feasibility of extracting new astrophysical findings from historical archival data.<\/p><\/div><br><div style=\"margin-left: 20px\"><i class=\"material-icons\" style='vertical-align: text-bottom'>record_voice_over<\/i> <b><span class=\"name\">Manja Zimmerer <\/span><\/b><br><span class=\"title\">Determining the Contribution of Massive Stars and Classical Novae to the Radioactive Isotope 26 Al<\/span><br><p class=\"abstract\">The isotopes 26Al and 60Fe show short lifetimes (\u223c 106 yr) with respect to the time scales of Galactic evolution and are therefore\r\nused as messengers of ongoing nucleosynthesis and star formation in the Milky Way. The production of both isotopes is commonly\r\nassociated with massive stars. They are thought to be ejected in their supernovae, and in the case of 26Al partially in the wind phase\r\nof the star. Because of their similar origin and lifetimes , the ratio 60Fe\/26Al of their \u03b3-ray emission would be independent of the true\r\nlocation and distribution of their source, and yields a chance to test the outcome of stellar evolution models. The expected results\r\nof 60Fe\/26Al for core-collapse supernovae, however, show discrepancies with measurements (Spyrou et al. 2024). This method only\r\nworks, if 26Al and 60Fe have the same origin throughout the Galaxy. At the same time recent results from 26 Al measurements suggest\r\na star formation rate (SFR) of \u2273 5 M\u2299\/yr (Siegert et al. 2023), which exceeds other literature values. Classical novae are also believed\r\nto produce 26 Al, which, if the contribution is large enough, would decrease the SFR from the correlation of 26 Al with massive stars.\r\nWe aim to determine the 26 Al mass as a function of Galactocentric radius and compare it with two Galactic chemical evolution (GCE)\r\nmodels (Vasini et al. 2025; Martinet et al. 2022) to estimate the contribution of (very) massive stars and classical novae. We are using\r\n20 yr of INTEGRAL\/SPI observations of the decay gamma-ray line at 1. 809 MeV to test different assumptions on the radial structure\r\nof 26 Al.\r\nWe present the total mass, the Galactic distribution of the 26Al, and the relative contribution of 26Al assuming different Galactic 3D\r\nmodels. We find significant contributions from classical novae which exceed prior studies for all tested models. A larger contribution\r\nof 26Al from classical novae directly decreases the effective 60Fe\/26Al ratio affects the interpretation as a probe of massive-star\r\nnucleosynthesis and would lower the SFR from 26Al \u03b3-ray measurements accordingly to 1-2 M\u2299\/yr<\/p><\/div><br><div style=\"margin-left: 20px\"><i class=\"material-icons\" style='vertical-align: text-bottom'>record_voice_over<\/i> <b><span class=\"name\">Vojt\u011bch \u0160imon <\/span><\/b><br><span class=\"title\">The variable recurrence times of outbursts in soft X-ray transients <\/span><br><p class=\"abstract\">Since the typical lengths of the recurrence times Tc (cycle lengths) of outbursts in soft X-ray transients (SXTs) range from months to decades, X-ray monitors are needed to detect them and investigate their evolution. Evolution of Tc shows a complex curve with episodes of increase and decrease. Significant results can be obtained even when different monitors with various energy bands, available for the individual time segments (years or decades), are used (e.g., ASM\/RXTE, MAXI\/ISS, BAT\/Swift). The character of the O-C curves of SXTs bears a striking similarity to that of dwarf novae observed in the optical band. It means that variations in Tc are large, but generally not chaotic, and long-term trends in the O-C curves can be resolved. Observing the variety of the X-ray evolution of dwarf novae is still limited by the low sensitivity of the current X-ray monitors.<\/p><\/div><br><h2 style='color: var(--conf-color-abstract-session);' id=\"GRB\">Gamma-Ray Bursts & Robotic Telescopes<span style='font-size: 18px; vertical-align: text-bottom; margin-left:20px;'> <i class=\"material-icons\" style=\"vertical-align: middle;\">record_voice_over<\/i> 1<\/span><\/h2><div style=\"margin-left: 20px\"><i class=\"material-icons\" style='vertical-align: text-bottom'>record_voice_over<\/i> <b><span class=\"name\">Martin Jel\u00ednek <\/span><\/b><br><span class=\"title\">Gamma Ray Bursts and Robotic Telescopes<\/span><br><p class=\"abstract\">Lorem ipsum dolor sit amet, consectetuer adipiscing elit. Aenean commodo ligula eget dolor. Aenean massa. Cum sociis natoque penatibus et magnis dis parturient montes, nascetur ridiculus mus. Donec quam felis, ultricies nec, pellentesque eu, pretium quis, sem. Nulla consequat massa quis enim. Donec pede justo, fringilla vel, aliquet nec, vulputate eget, arcu. In enim justo, rhoncus ut, imperdiet a, venenatis vitae, justo. Nullam dictum felis eu pede mollis pretium. Integer tincidunt. Cras dapibus. Vivamus elementum semper nisi. Aenean vulputate eleifend tellus. Aenean leo ligula, porttitor eu, consequat vitae, eleifend ac, enim. Aliquam lorem ante, dapibus in, viverra quis, feugiat a, tellus. Phasellus viverra nulla ut metus varius laoreet. Quisque rutrum. Aenean imperdiet. Etiam ultricies nisi vel augue. Curabitur ullamcorper ultricies nisi. Nam eget dui. Etiam rhoncus. Maecenas tempus, tellus eget condimentum rhoncus, sem quam semper libero, sit amet adipiscing sem neque sed ipsum. Nam quam nunc, blandit vel, luctus pulvinar, hendrerit id, lorem. Maecenas nec odio et ante tincidunt tempus. Donec vitae sapien ut libero venenatis faucibus. Nullam quis ante. Etiam sit amet orci eget eros faucibus tincidunt. Duis leo. Sed fringilla mauris sit amet nibh. Donec sodales sagittis magna. Sed consequat, leo eget bibendum sodales, augue velit cursus nunc,<\/p><\/div><br><h2 style='color: var(--conf-color-abstract-session);' id=\"SAT\">Small satellites & Instrumental session<span style='font-size: 18px; vertical-align: text-bottom; margin-left:20px;'> <i class=\"material-icons\" style=\"vertical-align: middle;\">record_voice_over<\/i> 4<\/span><\/h2><div style=\"margin-left: 20px\"><i class=\"material-icons\" style='vertical-align: text-bottom'>record_voice_over<\/i> <b><span class=\"name\">Ulvi Mehraliyev <\/span><\/b><br><span class=\"title\">MATHEMATICAL MODELLING OF A PIEZOELECTRIC ACCELEROMETER FOR AEROSPACE APPLICATION<\/span><br><p class=\"abstract\">Accelerometers are devices that sense acceleration and transmit it as an electrical signal to measurement units. Recently, accelerometers have made an important contributionto several fields such as aerospace, space, health monitoring, and other industries.This study is dedicated to the mathematical modelling and development of a newly developed three-axis piezoelectric accelerometer for space applications based on LEO CubeSat missions. The modelling, development, and required simulations are carried out using COMSOL Multiphysics software. The main objective of this work is to develop an easily manufacturable, cost-effective, and sensitive three-axis piezoelectric accelerometer for attitude determination systems in low Earth orbit based space applications.\r\n<\/p><\/div><br><div style=\"margin-left: 20px\"><i class=\"material-icons\" style='vertical-align: text-bottom'>record_voice_over<\/i> <b><span class=\"name\">Filip M\u00fcnz <\/span><\/b><br><span class=\"title\">QUVIK Science Operations<\/span><br><p class=\"abstract\">QUVIK is a Czech-led project of a small UV space telescope that has been selected and funded to be launched in year30\/31. Masaryk University will be primarily responsible for developing and running a Science Operation Center that has 2 main tasks: defining most scientifically valuable observation plan (taking into account constraints of Low Earth Orbit and the power budget) and creating the most performing data processing pipeline (with a very limited baseline of on-board data handling). Our experience of operations of small telescopes on ground (mostly run in automatized regime) is the pincipal ingredience in this development. First steps taken in the process closely supervised by ESA support team will be presented.<\/p><\/div><br><div style=\"margin-left: 20px\"><i class=\"material-icons\" style='vertical-align: text-bottom'>record_voice_over<\/i> <b><span class=\"name\">Klaus Schilling <\/span><\/b><br><span class=\"title\">Formations of Small Satellites Open Up New Application Fields<\/span><br><p class=\"abstract\">Technology progress for small satellites allows self-organizing multi-satellite systems for observations.  The satellite formation will be configured by miniature attitude and orbit control systems to optimize network properties. This potential is exploited in Earth observation regarding multi-perspective measurements. At the launch pad in California are currently multi-satellite missions from W\u00fcrzburg, such as \r\n  - TOM : 3 cooperating satellites to generate 3D surface images,\r\n  - CuBy : 5 satellites with multi-spectral cameras for biomonitoring and geodesy applications. \r\nTransfer of such formation principles to support astronomical observations offer good potential for innovative distributed sensing methods and will be jointly further explored during this workshop.<\/p><\/div><br><div style=\"margin-left: 20px\"><i class=\"material-icons\" style='vertical-align: text-bottom'>record_voice_over<\/i> <b><span class=\"name\">Vojt\u011bch \u0160imon <\/span><\/b><br><span class=\"title\">Astronomical observing with SXI\/SMILE <\/span><br><p class=\"abstract\">We show that a Soft X-ray Imager (SXI) onboard the ESA-CAS satellite SMILE will be able to observe various types of mass accreting compact objects in the universe. We show that mainly neutron stars accreting matter from their companions in X-ray binaries are promising targets for evaluating the possibilities of SXI in astronomical research. We present the typical features of the long-term activity of various X-ray binaries in the SXI\/SMILE field of view. We also show that binaries with steady-state thermonuclear reactions on board accreting white dwarfs in the Magellanic Clouds are promising targets for SXI observations. We discuss how SXI can contribute to this branch. \r\n<\/p><\/div><br><hr><span class=\"name\" style='color: var(--conf-color-abstract-text); vertical-align: text-bottom;'><i class=\"material-icons\" style=\"vertical-align: middle;\">record_voice_over<\/i> - Talks (15)\t<i class=\"material-icons\" style=\"vertical-align: middle;\">description<\/i> - Posters (0) <\/span>\n<p>[\/et_pb_text][\/et_pb_column][\/et_pb_row][\/et_pb_section][et_pb_section fb_built=&#8221;1&#8243; disabled_on=&#8221;on|on|on&#8221; admin_label=&#8221;Overview&#8221; _builder_version=&#8221;4.16&#8243; background_color=&#8221;#091744&#8243; background_image=&#8221;https:\/\/ibws.cz\/wp-content\/uploads\/2019\/11\/gaming-02.png&#8221; background_position=&#8221;top_center&#8221; disabled=&#8221;on&#8221; global_colors_info=&#8221;{}&#8221; box_shadow_style__hover=&#8221;none&#8221; box_shadow_style__hover_enabled=&#8221;none&#8221; box_shadow_color__hover=&#8221;rgba(0,0,0,0.3)&#8221; box_shadow_color__hover_enabled=&#8221;rgba(0,0,0,0.3)&#8221;][et_pb_row column_structure=&#8221;1_2,1_4,1_4&#8243; _builder_version=&#8221;4.16&#8243; locked=&#8221;off&#8221; global_colors_info=&#8221;{}&#8221;][et_pb_column type=&#8221;1_2&#8243; _builder_version=&#8221;4.16&#8243; custom_padding=&#8221;|||&#8221; global_colors_info=&#8221;{}&#8221; custom_padding__hover=&#8221;|||&#8221;][et_pb_divider color=&#8221;#14f1d9&#8243; divider_weight=&#8221;4px&#8221; _builder_version=&#8221;4.16&#8243; max_width=&#8221;80px&#8221; height=&#8221;4px&#8221; locked=&#8221;off&#8221; global_colors_info=&#8221;{}&#8221;][\/et_pb_divider][et_pb_text _builder_version=&#8221;4.16&#8243; text_font=&#8221;Lato||||||||&#8221; text_font_size=&#8221;16px&#8221; text_line_height=&#8221;2em&#8221; header_font=&#8221;||||||||&#8221; header_2_font=&#8221;Rubik|700||on|||||&#8221; header_2_font_size=&#8221;44px&#8221; header_2_letter_spacing=&#8221;1px&#8221; header_2_line_height=&#8221;1.3em&#8221; background_layout=&#8221;dark&#8221; header_2_font_size_tablet=&#8221;34px&#8221; header_2_font_size_phone=&#8221;24px&#8221; header_2_font_size_last_edited=&#8221;on|phone&#8221; locked=&#8221;off&#8221; global_colors_info=&#8221;{}&#8221; header_font_size__hover=&#8221;30px&#8221; header_font_size__hover_enabled=&#8221;30px&#8221; header_letter_spacing__hover=&#8221;0px&#8221; header_letter_spacing__hover_enabled=&#8221;0px&#8221; header_text_shadow_style__hover=&#8221;none&#8221; header_text_shadow_style__hover_enabled=&#8221;none&#8221; header_text_shadow_color__hover=&#8221;rgba(0,0,0,0.4)&#8221; header_text_shadow_color__hover_enabled=&#8221;rgba(0,0,0,0.4)&#8221;]<\/p>\n<h2>Game Overview<\/h2>\n<p>[\/et_pb_text][et_pb_button button_text=&#8221;Learn More&#8221; button_alignment=&#8221;left&#8221; _builder_version=&#8221;4.16&#8243; custom_button=&#8221;on&#8221; button_text_size=&#8221;14px&#8221; button_text_color=&#8221;#091744&#8243; button_bg_color=&#8221;#14f1d9&#8243; button_border_width=&#8221;0px&#8221; button_border_radius=&#8221;100px&#8221; button_letter_spacing=&#8221;1px&#8221; button_font=&#8221;Rubik|500||on|||||&#8221; custom_padding=&#8221;16px|40px|16px|40px|true|true&#8221; button_letter_spacing_last_edited=&#8221;off|desktop&#8221; box_shadow_style=&#8221;preset3&#8243; box_shadow_blur=&#8221;28px&#8221; box_shadow_color=&#8221;rgba(20,241,217,0.24)&#8221; locked=&#8221;off&#8221; global_colors_info=&#8221;{}&#8221; button_letter_spacing__hover=&#8221;2px&#8221; button_letter_spacing__hover_enabled=&#8221;on&#8221;][\/et_pb_button][\/et_pb_column][et_pb_column type=&#8221;1_4&#8243; _builder_version=&#8221;4.16&#8243; custom_padding=&#8221;|||&#8221; global_colors_info=&#8221;{}&#8221; custom_padding__hover=&#8221;|||&#8221;][et_pb_text _builder_version=&#8221;4.16&#8243; text_font=&#8221;Lato||||||||&#8221; text_font_size=&#8221;18px&#8221; text_line_height=&#8221;2em&#8221; header_font=&#8221;||||||||&#8221; header_3_font=&#8221;||||||||&#8221; header_4_font=&#8221;Rubik|500||on|||||&#8221; header_4_text_color=&#8221;#14f1d9&#8243; header_4_font_size=&#8221;11px&#8221; header_4_letter_spacing=&#8221;2px&#8221; background_layout=&#8221;dark&#8221; locked=&#8221;off&#8221; global_colors_info=&#8221;{}&#8221;]<\/p>\n<h4>Genre<\/h4>\n<p>Action, Adventure, Shooter<\/p>\n<p>[\/et_pb_text][et_pb_text _builder_version=&#8221;4.16&#8243; text_font=&#8221;Lato||||||||&#8221; text_font_size=&#8221;18px&#8221; text_line_height=&#8221;2em&#8221; header_font=&#8221;||||||||&#8221; header_3_font=&#8221;||||||||&#8221; header_4_font=&#8221;Rubik|500||on|||||&#8221; header_4_text_color=&#8221;#14f1d9&#8243; header_4_font_size=&#8221;11px&#8221; header_4_letter_spacing=&#8221;2px&#8221; background_layout=&#8221;dark&#8221; locked=&#8221;off&#8221; global_colors_info=&#8221;{}&#8221;]<\/p>\n<h4>Release Date<\/h4>\n<p>December 02, 2018<\/p>\n<p>[\/et_pb_text][\/et_pb_column][et_pb_column type=&#8221;1_4&#8243; _builder_version=&#8221;4.16&#8243; custom_padding=&#8221;|||&#8221; global_colors_info=&#8221;{}&#8221; custom_padding__hover=&#8221;|||&#8221;][et_pb_text _builder_version=&#8221;4.16&#8243; text_font=&#8221;Lato||||||||&#8221; text_font_size=&#8221;18px&#8221; text_line_height=&#8221;2em&#8221; header_font=&#8221;||||||||&#8221; header_3_font=&#8221;||||||||&#8221; header_4_font=&#8221;Rubik|500||on|||||&#8221; header_4_text_color=&#8221;#14f1d9&#8243; header_4_font_size=&#8221;11px&#8221; header_4_letter_spacing=&#8221;2px&#8221; background_layout=&#8221;dark&#8221; locked=&#8221;off&#8221; global_colors_info=&#8221;{}&#8221;]<\/p>\n<h4>Publisher<\/h4>\n<p>Elegant Themes<\/p>\n<p>[\/et_pb_text][et_pb_text _builder_version=&#8221;4.16&#8243; text_font=&#8221;Lato||||||||&#8221; text_font_size=&#8221;18px&#8221; text_line_height=&#8221;2em&#8221; header_font=&#8221;||||||||&#8221; header_3_font=&#8221;||||||||&#8221; header_4_font=&#8221;Rubik|500||on|||||&#8221; header_4_text_color=&#8221;#14f1d9&#8243; header_4_font_size=&#8221;11px&#8221; header_4_letter_spacing=&#8221;2px&#8221; background_layout=&#8221;dark&#8221; locked=&#8221;off&#8221; global_colors_info=&#8221;{}&#8221;]<\/p>\n<h4>Platforms<\/h4>\n<p>WordPress, Divi<\/p>\n<p>[\/et_pb_text][\/et_pb_column][\/et_pb_row][et_pb_row column_structure=&#8221;1_2,1_2&#8243; _builder_version=&#8221;4.16&#8243; custom_margin=&#8221;||8vw&#8221; custom_padding=&#8221;0|0px|27px|0px|false|false&#8221; global_colors_info=&#8221;{}&#8221;][et_pb_column type=&#8221;1_2&#8243; _builder_version=&#8221;4.16&#8243; custom_padding=&#8221;|||&#8221; global_colors_info=&#8221;{}&#8221; custom_padding__hover=&#8221;|||&#8221;][\/et_pb_column][et_pb_column type=&#8221;1_2&#8243; _builder_version=&#8221;4.16&#8243; custom_padding=&#8221;|||&#8221; global_colors_info=&#8221;{}&#8221; custom_padding__hover=&#8221;|||&#8221;][et_pb_text _builder_version=&#8221;4.16&#8243; text_font=&#8221;Lato||||||||&#8221; text_text_color=&#8221;#9fa5d6&#8243; text_font_size=&#8221;16px&#8221; text_line_height=&#8221;2em&#8221; background_layout=&#8221;dark&#8221; locked=&#8221;off&#8221; global_colors_info=&#8221;{}&#8221;]<\/p>\n<p>Sed porttitor lectus nibh. Mauris blandit aliquet elit, eget tincidunt nibh pulvinar a. Vivamus suscipit tortor eget felis porttitor volutpat. Proin eget tortor risus. Cras ultricies ligula sed magna dictum porta. Donec rutrum congue leo eget malesuada. Vestibulum ante ipsum primis in faucibus orci luctus et ultrices posuere cubilia Curae; Donec velit neque, auctor sit amet aliquam vel, ullamcorper sit amet ligula. Vestibulum ante ipsum primis in faucibus orci luctus et ultrices posuere cubilia Curae; Donec velit neque, auctor sit amet aliquam vel, ullamcorper sit amet ligula. Vestibulum ante ipsum primis in faucibus orci luctus et ultrices posuere cubilia Curae; Donec velit neque, auctor sit a<\/p>\n<p>[\/et_pb_text][\/et_pb_column][\/et_pb_row][et_pb_row _builder_version=&#8221;4.16&#8243; locked=&#8221;off&#8221; global_colors_info=&#8221;{}&#8221;][et_pb_column type=&#8221;4_4&#8243; _builder_version=&#8221;4.16&#8243; custom_padding=&#8221;|||&#8221; global_colors_info=&#8221;{}&#8221; custom_padding__hover=&#8221;|||&#8221;][et_pb_divider color=&#8221;#14f1d9&#8243; divider_weight=&#8221;4px&#8221; _builder_version=&#8221;4.16&#8243; max_width=&#8221;80px&#8221; module_alignment=&#8221;center&#8221; height=&#8221;4px&#8221; locked=&#8221;off&#8221; global_colors_info=&#8221;{}&#8221;][\/et_pb_divider][et_pb_text _builder_version=&#8221;4.16&#8243; text_font=&#8221;Lato||||||||&#8221; text_text_color=&#8221;#9fa5d6&#8243; text_font_size=&#8221;16px&#8221; text_line_height=&#8221;2em&#8221; header_2_font=&#8221;Rubik|700||on|||||&#8221; header_2_font_size=&#8221;44px&#8221; header_2_letter_spacing=&#8221;1px&#8221; header_2_line_height=&#8221;1.3em&#8221; text_orientation=&#8221;center&#8221; background_layout=&#8221;dark&#8221; max_width=&#8221;700px&#8221; module_alignment=&#8221;center&#8221; header_2_font_size_tablet=&#8221;34px&#8221; header_2_font_size_phone=&#8221;24px&#8221; header_2_font_size_last_edited=&#8221;on|phone&#8221; locked=&#8221;off&#8221; global_colors_info=&#8221;{}&#8221; header_font_size__hover=&#8221;30px&#8221; header_font_size__hover_enabled=&#8221;30px&#8221; header_letter_spacing__hover=&#8221;0px&#8221; header_letter_spacing__hover_enabled=&#8221;0px&#8221; header_text_shadow_style__hover=&#8221;none&#8221; header_text_shadow_style__hover_enabled=&#8221;none&#8221; header_text_shadow_color__hover=&#8221;rgba(0,0,0,0.4)&#8221; header_text_shadow_color__hover_enabled=&#8221;rgba(0,0,0,0.4)&#8221;]<\/p>\n<h2>Game Features<\/h2>\n<p>Mauris blandit aliquet elit, eget tincidunt nibh pulvinar a. Nulla quis lorem ut libero malesuada feugiat. Nulla quis lorem ut libero malesuada feugiat. Nulla quis lorem ut libero m<\/p>\n<p>[\/et_pb_text][et_pb_button button_text=&#8221;Video Walk-Through&#8221; button_alignment=&#8221;center&#8221; _builder_version=&#8221;4.16&#8243; custom_button=&#8221;on&#8221; button_text_size=&#8221;14px&#8221; button_text_color=&#8221;#091744&#8243; button_bg_color=&#8221;#14f1d9&#8243; button_border_width=&#8221;0px&#8221; button_border_radius=&#8221;100px&#8221; button_letter_spacing=&#8221;1px&#8221; button_font=&#8221;Rubik|500||on|||||&#8221; custom_padding=&#8221;16px|40px|16px|40px|true|true&#8221; button_letter_spacing_last_edited=&#8221;off|desktop&#8221; box_shadow_style=&#8221;preset3&#8243; box_shadow_blur=&#8221;28px&#8221; box_shadow_color=&#8221;rgba(20,241,217,0.24)&#8221; locked=&#8221;off&#8221; global_colors_info=&#8221;{}&#8221; button_letter_spacing__hover=&#8221;2px&#8221; button_letter_spacing__hover_enabled=&#8221;on&#8221;][\/et_pb_button][\/et_pb_column][\/et_pb_row][et_pb_row column_structure=&#8221;1_3,1_3,1_3&#8243; padding_left_right_link_1=&#8221;true&#8221; padding_left_right_link_2=&#8221;true&#8221; padding_left_right_link_3=&#8221;true&#8221; _builder_version=&#8221;4.16&#8243; animation_style=&#8221;slide&#8221; animation_direction=&#8221;bottom&#8221; animation_intensity_slide=&#8221;10%&#8221; global_colors_info=&#8221;{}&#8221;][et_pb_column type=&#8221;1_3&#8243; _builder_version=&#8221;4.16&#8243; background_image=&#8221;https:\/\/ibws.cz\/wp-content\/uploads\/2019\/11\/gaming-01.png&#8221; background_size=&#8221;contain&#8221; background_position=&#8221;top_center&#8221; custom_padding=&#8221;100px|30px||30px&#8221; global_colors_info=&#8221;{}&#8221; custom_padding__hover=&#8221;|||&#8221;][et_pb_blurb title=&#8221;Aliquam Tincidunt&#8221; image=&#8221;https:\/\/ibws.cz\/wp-content\/uploads\/2019\/11\/gaming-icon-05.png&#8221; _builder_version=&#8221;4.16&#8243; header_font=&#8221;Rubik||||||||&#8221; header_line_height=&#8221;1.6em&#8221; body_font=&#8221;Lato||||||||&#8221; body_text_color=&#8221;#9fa5d6&#8243; body_line_height=&#8221;1.9em&#8221; text_orientation=&#8221;center&#8221; background_layout=&#8221;dark&#8221; animation=&#8221;off&#8221; locked=&#8221;off&#8221; global_colors_info=&#8221;{}&#8221;]<\/p>\n<p>Proin eget tortor risus. Donec rutrum congue leo eget malesuada. 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This is especially the case for Black Hole X-ray Binaries (BHXB), also known as Microquasars, for which many unresolved challenges remain. In particular acceleration mechanisms and how they relate to accretion-ejection processes. Combined with spectroscopy, polarization is a powerful tool to reveal the geometry of the system and the configuration of the magnetic fields.\r\n\r\nThe persistent Microquasar Cygnus X-1 is particularly well suited for our analysis. In soft X-rays, the polarization is low and aligned with the general direction of the jet, while the polarization angle in the soft gamma-rays is found close to 70\u00b0 away from the jet. We use a novel method to combine high-energy spectra and polarization of this bright source from 1 keV to 2 MeV in a single fit, including observations from IXPE, PoGO+, XL-Calibur, AstroSat, INTEGRAL\/SPI and INTEGRAL\/IBIS. Our study involves energy-dependent polarization models for both emission processes, in part inspired by similar studies on Blazars.\r\n\r\nPreliminary results already reveal new constraints about the non-thermal hard-tail origin (above 100 keV), in particular its high-energy spectral cut-off and the degree of order of the magnetic field.<\/p><\/div><br><div style=\"margin-left: 20px\"><i class=\"material-icons\" style='vertical-align: text-bottom'>record_voice_over<\/i> <b><span class=\"name\">Rene Hudec <\/span><\/b><br><span class=\"title\">IBWS Introduction and Historical Backgroundf<\/span><br><p class=\"abstract\">Originally, the IBWS (INTEGRAL\/BART) workshops focused on the work of High energy\r\nastrophysics group (at that dime dominated by young research fellows and students) in\r\nAstronomical Institute of the Academy of Sciences of the Czech Republic and relevant\r\nnational and international collaborators from the field, with intensive student participation.\r\nDuring the early years, these activities were focussed on the ESA INTEGRAL satellite and\r\non the related ground-based robotic telescopes, e.g. the small robotic BART telescope\r\nat the Ondrejov Observatory.\r\nNowadays, the IBWS workshops promote regional collaboration in galactic and\r\nextragalactic high-energy astrophysics, both experimental as well as theoretical, with an\r\nemphasis on the interface between satellite projects and ground-based experiments (e.g.\r\nrobotic telescopes). We continue our emphasis on wide participation and presentations of\r\nstudents and young research fellows.<\/p><\/div><br><div style=\"margin-left: 20px\"><i class=\"material-icons\" style='vertical-align: text-bottom'>record_voice_over<\/i> <b><span class=\"name\">Bendeg\u00faz Koncz <\/span><\/b><br><span class=\"title\">Galaxy mergers history in the IllustrisTNG simulation<\/span><br><p class=\"abstract\">Galaxy evolution over time remains unclear, with ongoing debate about how collisions affect star formation and metallicity. The role of the local environment shaped by the large-scale structure of the Universe in galaxy mergers may be significant, yet it has not been thoroughly examined. Using the IllustrisTNG cosmological simulation, we processed the catalog data and merger tree files of the TNG300-1 run. We calculated the average star formation rate (SFR) and stellar mass of galaxies over the redshift range 0 < z < 15 to trace the cosmic star formation history and galaxy growth. We investigated the environments of galaxy mergers with a focus on local density within the cosmic web, and found that interactions with gas-rich dwarf galaxies can trigger a resurgence in gas supply, highlighting the importance of gas dynamics in sustaining star formation. We compared our results with recent JWST observations and identified differences in the star formation rate density (SFRD) history between simulations and observations, providing new insights into early galaxy formation and evolution. See Koncz et. al. Universe 2025, 11(9), 286.<\/p><\/div><br><div style=\"margin-left: 20px\"><i class=\"material-icons\" style='vertical-align: text-bottom'>record_voice_over<\/i> <b><span class=\"name\">Saurabh Mittal <\/span><\/b><br><span class=\"title\">Contribution of Stellar flares to the 511 keV Galactic positron budget<\/span><br><p class=\"abstract\">The origin of the Galactic 511 keV positron annihilation line has been a mystery for five decades. One proposed explanation is positron production in stellar flares, motivated by the detection of the 511 keV line in solar flares and by the association of this emission with old stellar populations. In this work, we explore this scenario using two complementary approaches. First, we build a theoretical model to estimate the quasi-persistent 511 keV emission from flaring stars. Starting from solar flare observations, we construct empirical scaling relations between flare energy and 511 keV luminosity and extend them to Galactic stellar populations using flare-frequency-energy distributions for different spectral types. In parallel, we analyze INTEGRAL\/SPI data in the 511 keV band using combinations of known point sources and simple spatial templates, such as disk and bulge components modeled as two-dimensional Gaussians. We also test alternative descriptions in which no bulge template is assumed and the emission is instead described by a disk component together with a population of globular clusters, scaled by their masses and distances. This ongoing work aims to assess whether stellar flares can plausibly account for the observed Galactic 511 keV emission.<\/p><\/div><br><div style=\"margin-left: 20px\"><i class=\"material-icons\" style='vertical-align: text-bottom'>record_voice_over<\/i> <b><span class=\"name\">Ondrej Pejcha <\/span><\/b><br><span class=\"title\">Evolution of binary stars leading up to high-energy sources<\/span><br><p class=\"abstract\">Many stellar high-energy sources are manifestations of one of the stages of binary star evolution. In this talk, I will discuss the astrophysical processes influencing binary star evolution such as mass transfer and the response of mass-losing and mass-accreting stars, formation of circumbinary medium, explosions, and violent events such as common envelope evolution, as well as their relation to end products such as gravitational wave sources. I will cover in greater detail two types of transient events: luminous red novae, which accompany stellar mergers and potentially hold the key to connecting many different evolutionary pathways , and classical novae, where recent GeV Fermi detections as well as ground, space, and interferometric observations suggest a much more complicated picture of mass ejection than previously thought.<\/p><\/div><br><div style=\"margin-left: 20px\"><i class=\"material-icons\" style='vertical-align: text-bottom'>record_voice_over<\/i> <b><span class=\"name\">Thomas Siegert <\/span><\/b><br><span class=\"title\">Nuclear Astrophysics and Gamma-Rays:\u2028From Space to Earth<\/span><br><p class=\"abstract\">Gamma rays provide a unique window on nuclear processes occurring throughout the Universe, directly tracing radioactive isotopes and matter antimatter annihilation.\r\nIn this talk, I will review key results from gamma-ray line spectroscopy in space, focusing on observations from 22 years of the now completed ESA satellite mission INTEGRAL. Measurements of radioactive isotopes, such as 26Al and 60Fe, reveal ongoing nucleosynthesis in the Galaxy and connect stellar explosions to traces found on Earth, including signatures preserved in ocean crust sediments. In this context, the long-standing puzzle of the Galactic 511 keV positron annihilation emission is also discussed.\r\nNASA\u2019s Compton Spectrometer and Imager (COSI) mission, scheduled for launch in 2027, is expected to significantly advance MeV measurements thanks to its increased sensitivity and imaging capabilities. I will introduce the Compton telescope concept and highlight open questions addressed by COSI, such as the role of massive stars and supernovae in Galactic feedback.\r\nFinally, I will show how analysis and imaging techniques developed for space-based gamma-ray astronomy are now being applied on Earth, enabling isotopic imaging of radioactive residues in nuclear facilities and related environments.<\/p><\/div><br><div style=\"margin-left: 20px\"><i class=\"material-icons\" style='vertical-align: text-bottom'>record_voice_over<\/i> <b><span class=\"name\">N\u00f3ra Varga <\/span><\/b><br><span class=\"title\">The Potential of the THESEUS Mission for Studies of Young Stellar Objects<\/span><br><p class=\"abstract\">The Transient High-Energy Sky and Early Universe Surveyor (THESEUS) is a space mission concept designed to perform repeated wide-area surveys of the sky, primarily to detect and characterize high-redshift gamma-ray bursts. As a consequence of its baseline observing strategy, THESEUS will also provide systematic, time-dependent coverage of large fractions of the sky in the soft X-ray and near-infrared domains, offering new opportunities for studies of Galactic sources beyond its core cosmological goals.\r\nWe aim to assess the observability of nearby star-forming regions and young stellar objects (YSOs) within the baseline survey strategy of THESEUS. We investigate how the mission\u2019s pointing concept and sky-coverage pattern translate into the temporal visibility of prominent nearby star-forming complexes and how this visibility is distributed over the mission lifetime. <\/p><\/div><br><div style=\"margin-left: 20px\"><i class=\"material-icons\" style='vertical-align: text-bottom'>record_voice_over<\/i> <b><span class=\"name\">Tauseef Ahmad Zafar <\/span><\/b><br><span class=\"title\">Data mining in astronomical photographic archives with advanced IT methods<\/span><br><p class=\"abstract\">We report on recent progress in the digitization of astronomical plate archives and the application of novel IT approaches, including machine learning methods, to these data. Astronomical photographic archives represent an extensive and largely untapped database of stellar, solar, and planetary observations, encompassing astrometric, photometric, and spectroscopic measurements accumulated over more than a century. These archives hold significant potential for a wide range of applications in modern astrophysics, including the study of long-term variability, detection of rare transient events, and identification of objects with peculiar spectra. We present results from visits to over 16 US institutions and numerous European, Mexican, and Chinese observatories, where plate samples were digitized using a transportable scanning device. We further describe the application of advanced computational techniques to digitized plates from the Sonneberg Observatory and the Henize Mt. Wilson Michigan Southern Sky Survey, demonstrating the feasibility of extracting new astrophysical findings from historical archival data.<\/p><\/div><br><div style=\"margin-left: 20px\"><i class=\"material-icons\" style='vertical-align: text-bottom'>record_voice_over<\/i> <b><span class=\"name\">Manja Zimmerer <\/span><\/b><br><span class=\"title\">Determining the Contribution of Massive Stars and Classical Novae to the Radioactive Isotope 26 Al<\/span><br><p class=\"abstract\">The isotopes 26Al and 60Fe show short lifetimes (\u223c 106 yr) with respect to the time scales of Galactic evolution and are therefore\r\nused as messengers of ongoing nucleosynthesis and star formation in the Milky Way. The production of both isotopes is commonly\r\nassociated with massive stars. They are thought to be ejected in their supernovae, and in the case of 26Al partially in the wind phase\r\nof the star. Because of their similar origin and lifetimes , the ratio 60Fe\/26Al of their \u03b3-ray emission would be independent of the true\r\nlocation and distribution of their source, and yields a chance to test the outcome of stellar evolution models. The expected results\r\nof 60Fe\/26Al for core-collapse supernovae, however, show discrepancies with measurements (Spyrou et al. 2024). This method only\r\nworks, if 26Al and 60Fe have the same origin throughout the Galaxy. At the same time recent results from 26 Al measurements suggest\r\na star formation rate (SFR) of \u2273 5 M\u2299\/yr (Siegert et al. 2023), which exceeds other literature values. Classical novae are also believed\r\nto produce 26 Al, which, if the contribution is large enough, would decrease the SFR from the correlation of 26 Al with massive stars.\r\nWe aim to determine the 26 Al mass as a function of Galactocentric radius and compare it with two Galactic chemical evolution (GCE)\r\nmodels (Vasini et al. 2025; Martinet et al. 2022) to estimate the contribution of (very) massive stars and classical novae. We are using\r\n20 yr of INTEGRAL\/SPI observations of the decay gamma-ray line at 1. 809 MeV to test different assumptions on the radial structure\r\nof 26 Al.\r\nWe present the total mass, the Galactic distribution of the 26Al, and the relative contribution of 26Al assuming different Galactic 3D\r\nmodels. We find significant contributions from classical novae which exceed prior studies for all tested models. A larger contribution\r\nof 26Al from classical novae directly decreases the effective 60Fe\/26Al ratio affects the interpretation as a probe of massive-star\r\nnucleosynthesis and would lower the SFR from 26Al \u03b3-ray measurements accordingly to 1-2 M\u2299\/yr<\/p><\/div><br><div style=\"margin-left: 20px\"><i class=\"material-icons\" style='vertical-align: text-bottom'>record_voice_over<\/i> <b><span class=\"name\">Vojt\u011bch \u0160imon <\/span><\/b><br><span class=\"title\">The variable recurrence times of outbursts in soft X-ray transients <\/span><br><p class=\"abstract\">Since the typical lengths of the recurrence times Tc (cycle lengths) of outbursts in soft X-ray transients (SXTs) range from months to decades, X-ray monitors are needed to detect them and investigate their evolution. Evolution of Tc shows a complex curve with episodes of increase and decrease. Significant results can be obtained even when different monitors with various energy bands, available for the individual time segments (years or decades), are used (e.g., ASM\/RXTE, MAXI\/ISS, BAT\/Swift). The character of the O-C curves of SXTs bears a striking similarity to that of dwarf novae observed in the optical band. It means that variations in Tc are large, but generally not chaotic, and long-term trends in the O-C curves can be resolved. Observing the variety of the X-ray evolution of dwarf novae is still limited by the low sensitivity of the current X-ray monitors.<\/p><\/div><br><h2 style='color: var(--conf-color-abstract-session);' id=\"GRB\">Gamma-Ray Bursts & Robotic Telescopes<span style='font-size: 18px; vertical-align: text-bottom; margin-left:20px;'> <i class=\"material-icons\" style=\"vertical-align: middle;\">record_voice_over<\/i> 1<\/span><\/h2><div style=\"margin-left: 20px\"><i class=\"material-icons\" style='vertical-align: text-bottom'>record_voice_over<\/i> <b><span class=\"name\">Martin Jel\u00ednek <\/span><\/b><br><span class=\"title\">Gamma Ray Bursts and Robotic Telescopes<\/span><br><p class=\"abstract\">Lorem ipsum dolor sit amet, consectetuer adipiscing elit. Aenean commodo ligula eget dolor. Aenean massa. Cum sociis natoque penatibus et magnis dis parturient montes, nascetur ridiculus mus. Donec quam felis, ultricies nec, pellentesque eu, pretium quis, sem. Nulla consequat massa quis enim. Donec pede justo, fringilla vel, aliquet nec, vulputate eget, arcu. In enim justo, rhoncus ut, imperdiet a, venenatis vitae, justo. Nullam dictum felis eu pede mollis pretium. Integer tincidunt. Cras dapibus. Vivamus elementum semper nisi. Aenean vulputate eleifend tellus. Aenean leo ligula, porttitor eu, consequat vitae, eleifend ac, enim. Aliquam lorem ante, dapibus in, viverra quis, feugiat a, tellus. Phasellus viverra nulla ut metus varius laoreet. Quisque rutrum. Aenean imperdiet. Etiam ultricies nisi vel augue. Curabitur ullamcorper ultricies nisi. Nam eget dui. Etiam rhoncus. Maecenas tempus, tellus eget condimentum rhoncus, sem quam semper libero, sit amet adipiscing sem neque sed ipsum. Nam quam nunc, blandit vel, luctus pulvinar, hendrerit id, lorem. Maecenas nec odio et ante tincidunt tempus. Donec vitae sapien ut libero venenatis faucibus. Nullam quis ante. Etiam sit amet orci eget eros faucibus tincidunt. Duis leo. Sed fringilla mauris sit amet nibh. Donec sodales sagittis magna. Sed consequat, leo eget bibendum sodales, augue velit cursus nunc,<\/p><\/div><br><h2 style='color: var(--conf-color-abstract-session);' id=\"SAT\">Small satellites & Instrumental session<span style='font-size: 18px; vertical-align: text-bottom; margin-left:20px;'> <i class=\"material-icons\" style=\"vertical-align: middle;\">record_voice_over<\/i> 4<\/span><\/h2><div style=\"margin-left: 20px\"><i class=\"material-icons\" style='vertical-align: text-bottom'>record_voice_over<\/i> <b><span class=\"name\">Ulvi Mehraliyev <\/span><\/b><br><span class=\"title\">MATHEMATICAL MODELLING OF A PIEZOELECTRIC ACCELEROMETER FOR AEROSPACE APPLICATION<\/span><br><p class=\"abstract\">Accelerometers are devices that sense acceleration and transmit it as an electrical signal to measurement units. Recently, accelerometers have made an important contributionto several fields such as aerospace, space, health monitoring, and other industries.This study is dedicated to the mathematical modelling and development of a newly developed three-axis piezoelectric accelerometer for space applications based on LEO CubeSat missions. The modelling, development, and required simulations are carried out using COMSOL Multiphysics software. The main objective of this work is to develop an easily manufacturable, cost-effective, and sensitive three-axis piezoelectric accelerometer for attitude determination systems in low Earth orbit based space applications.\r\n<\/p><\/div><br><div style=\"margin-left: 20px\"><i class=\"material-icons\" style='vertical-align: text-bottom'>record_voice_over<\/i> <b><span class=\"name\">Filip M\u00fcnz <\/span><\/b><br><span class=\"title\">QUVIK Science Operations<\/span><br><p class=\"abstract\">QUVIK is a Czech-led project of a small UV space telescope that has been selected and funded to be launched in year30\/31. Masaryk University will be primarily responsible for developing and running a Science Operation Center that has 2 main tasks: defining most scientifically valuable observation plan (taking into account constraints of Low Earth Orbit and the power budget) and creating the most performing data processing pipeline (with a very limited baseline of on-board data handling). Our experience of operations of small telescopes on ground (mostly run in automatized regime) is the pincipal ingredience in this development. First steps taken in the process closely supervised by ESA support team will be presented.<\/p><\/div><br><div style=\"margin-left: 20px\"><i class=\"material-icons\" style='vertical-align: text-bottom'>record_voice_over<\/i> <b><span class=\"name\">Klaus Schilling <\/span><\/b><br><span class=\"title\">Formations of Small Satellites Open Up New Application Fields<\/span><br><p class=\"abstract\">Technology progress for small satellites allows self-organizing multi-satellite systems for observations.  The satellite formation will be configured by miniature attitude and orbit control systems to optimize network properties. This potential is exploited in Earth observation regarding multi-perspective measurements. At the launch pad in California are currently multi-satellite missions from W\u00fcrzburg, such as \r\n  - TOM : 3 cooperating satellites to generate 3D surface images,\r\n  - CuBy : 5 satellites with multi-spectral cameras for biomonitoring and geodesy applications. \r\nTransfer of such formation principles to support astronomical observations offer good potential for innovative distributed sensing methods and will be jointly further explored during this workshop.<\/p><\/div><br><div style=\"margin-left: 20px\"><i class=\"material-icons\" style='vertical-align: text-bottom'>record_voice_over<\/i> <b><span class=\"name\">Vojt\u011bch \u0160imon <\/span><\/b><br><span class=\"title\">Astronomical observing with SXI\/SMILE <\/span><br><p class=\"abstract\">We show that a Soft X-ray Imager (SXI) onboard the ESA-CAS satellite SMILE will be able to observe various types of mass accreting compact objects in the universe. We show that mainly neutron stars accreting matter from their companions in X-ray binaries are promising targets for evaluating the possibilities of SXI in astronomical research. We present the typical features of the long-term activity of various X-ray binaries in the SXI\/SMILE field of view. We also show that binaries with steady-state thermonuclear reactions on board accreting white dwarfs in the Magellanic Clouds are promising targets for SXI observations. We discuss how SXI can contribute to this branch. \r\n<\/p><\/div><br><hr><span class=\"name\" style='color: var(--conf-color-abstract-text); vertical-align: text-bottom;'><i class=\"material-icons\" style=\"vertical-align: middle;\">record_voice_over<\/i> - Talks (15)\t<i class=\"material-icons\" style=\"vertical-align: middle;\">description<\/i> - Posters (0) <\/span>Game OverviewGenre Action, Adventure, ShooterRelease Date December 02, 2018Publisher Elegant ThemesPlatforms WordPress, DiviSed porttitor lectus nibh. Mauris blandit aliquet elit, eget tincidunt nibh pulvinar a. Vivamus suscipit tortor eget felis porttitor volutpat. Proin eget tortor risus. Cras ultricies ligula sed magna dictum porta. Donec rutrum congue leo eget malesuada. 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