BEGIN:VCALENDAR VERSION:2.0 PRODID:-//CERN//INDICO//EN BEGIN:VEVENT SUMMARY:Limiting the number density of ultra-high-energy cosmic ray source s DTSTART;VALUE=DATE-TIME:20261030T143000Z DTEND;VALUE=DATE-TIME:20261030T144500Z DTSTAMP;VALUE=DATE-TIME:20261021T104106Z UID:indico-contribution-316-6218@cern.ch DESCRIPTION:Speakers: Pavliuk Anastasia (MIPT\, LPI\, JNR)\nThe origin of ultra-high-energy cosmic rays (UHECRs) remains an open problem. In particu lar\, the properties of their sources are difficult to constrain due to th e limited statistics of observed events and the propagation effects experi enced by charged cosmic rays. One of the important characteristics of sour ces is their number density. In this work\, we investigate the possibility of constraining the number density of UHECR sources using statistical pro perties of experimentally observed cosmic-ray events.\n\nThe analysis is b ased on public data from the Pierre Auger Observatory. We simulate UHECR e vents as they would be observed at Earth for different assumptions about t he primary composition\, source number density\, and energy threshold. For each set of parameters\, ensembles of simulated event sets are generated and compared with the experimental data. The simulations account for the m ain effects relevant to the propagation and detection of UHECRs.\n\nSevera l statistical methods are used to quantify the compatibility between the s imulated event sets and the experimental data. In particular\, we consider the two-point angular autocorrelation function\, which characterizes the clustering of events on different angular scales. The distributions of the corresponding statistics obtained from the simulated event sets are compa red with the values measured in the experimental data. \n\nThe preliminary results show that\, for most of the considered primary compositions and e nergy thresholds\, the simulated event sets are inconsistent with the expe rimental data across the investigated range of source densities.\n\nhttps: //indico.particle.mephi.ru/event/626/contributions/6218/ LOCATION:Sevastopol Hotel URL:https://indico.particle.mephi.ru/event/626/contributions/6218/ END:VEVENT BEGIN:VEVENT SUMMARY:ANALYSIS OF THE ELECTRON-PHOTON AND HADRON COMPONENTS OF EXTENSIVE AIR SHOWERS ACCORDING TO THE DATA OF THE NEVOD-EAS AND PRISMA-32 INSTALLA TIONS DTSTART;VALUE=DATE-TIME:20261030T151500Z DTEND;VALUE=DATE-TIME:20261030T153000Z DTSTAMP;VALUE=DATE-TIME:20261021T104106Z UID:indico-contribution-316-6219@cern.ch DESCRIPTION:Speakers: Elena Yuzhakova (MEPhI)\nAt the Experimental Complex NEVOD (EC NEVOD\, MEPhI\, Moscow)\, a technique for the simultaneous meas urement of the electron-photon and hadron components of extensive air show ers (EAS) has been implemented. The electron-photon component is detected by 36 scintillation detector stations of the NEVOD-EAS array\, arranged in 9 clusters and deployed on the roofs of the buildings and on the ground s urrounding them. The hadron component of the shower is detected through th ermal neutrons by the PRISMA-32 array\, located beneath the roof of EC NEV OD and consisting of two clusters of 16 en-detectors each. This detectors are capable of measuring both the charged component and the thermalized ne utrons produced in hadronic interactions of the shower core with the matte r surrounding the array.\nThe report presents a comparison of the characte ristics of the two EAS components based on joint data from both arrays. La teral distribution functions of thermal neutrons are obtained for differen t ranges of shower size. The results of the analysis of the ratio between the hadron and electron-photon components in the region of the knee of the cosmic ray energy spectrum are presented.\n\nhttps://indico.particle.meph i.ru/event/626/contributions/6219/ LOCATION:Sevastopol Hotel URL:https://indico.particle.mephi.ru/event/626/contributions/6219/ END:VEVENT BEGIN:VEVENT SUMMARY:Analysis of energy deposit of EAS cores in the Cherenkov water cal orimeter NEVOD DTSTART;VALUE=DATE-TIME:20261030T153000Z DTEND;VALUE=DATE-TIME:20261030T154500Z DTSTAMP;VALUE=DATE-TIME:20261021T104106Z UID:indico-contribution-316-6220@cern.ch DESCRIPTION:Speakers: Михаил Лисицин (PhD student)\nA basis o f the Experimental Complex NEVOD (MEPhI\, Moscow) is the Cherenkov water c alorimeter (CWC) with a volume of 2000 m3. The quasi-spherical modules (QS Ms) consisting of 6 orthogonally oriented photomultiplier tubes (PMTs) are used to detect Cherenkov radiation. The CWC NEVOD includes 91 QSMs (546 P MTs in total) which form a spatial grid in the water volume with 25 vertic ally arranged strings\, 3 – 4 QSMs in each. Such arrangement of photomul tiplier tubes and their wide dynamic range from 1 to 105 photoelectrons\, achieved by a two-dynode signal readout\, allows CWC NEVOD to operate in t he calorimeter mode.\n\nThe NEVOD-EAS array is a part of the Experimental Complex NEVOD. It consists of 36 scintillation detector stations (DS)\, co mbined into 9 clusters\, which are placed over an area of about 104 m2 on the roofs of laboratory buildings and on the ground surface. The array is designed to measure the electron-photon component of extensive air showers (EAS) within an energy range from 1015 to 1017 eV. Using its data various EAS parameters are reconstructed: the air-shower core position\, size and arrival direction.\n\nThe central part of an extensive air shower near it s axis is called the EAS core\, where hadrons being generated. In their de cays\, the hadrons form electron-photon and muon components of the EAS. Fl uctuations in the recorded shower characteristics\, containing information on primary nuclear interaction acts\, are minimal in the cores of extensi ve air showers. But at the same time\, most of the conducted studies are f ocused on the EAS electron-photon component\, which is the easiest one to detect.\n\nThe combination of the EC NEVOD facilities provides an opportun ity to select and reconstruct extensive air showers by the electron-photon component with NEVOD-EAS array and to study the energy deposit of EAS cor es in the Cherenkov water calorimeter.\n\nIn this work\, the study of join t events of the CWC NEVOD and the NEVOD-EAS array was carried out based on the experimental data recorded in 2018 - 2023. For such events\, the sele ction conditions and characteristics are presented\, the features of the r econstructed EAS size spectrum\, as well as the spectra of energy deposit from all events and events with cores passing through the CWC are discusse d.\n\nhttps://indico.particle.mephi.ru/event/626/contributions/6220/ LOCATION:Sevastopol Hotel URL:https://indico.particle.mephi.ru/event/626/contributions/6220/ END:VEVENT BEGIN:VEVENT SUMMARY:UHECR mass composition from their anisotropy with Telescope Array and Pierre Auger DTSTART;VALUE=DATE-TIME:20261030T141500Z DTEND;VALUE=DATE-TIME:20261030T143000Z DTSTAMP;VALUE=DATE-TIME:20261021T104106Z UID:indico-contribution-316-6221@cern.ch DESCRIPTION:Speakers: Mikhail Kuznetsov (INR\, Moscow)\nWe use a new metho d of ultra-high energy cosmic rays anisotropy analysis to infer their inje cted mass composition from the data. We use the data of the Telescope Arra y experiment and public data of the Pierre Auger experiment. Our results s how that a light composition is disfavored at all energies above 10 EeV\, unless the extragalactic magnetic field is extremely strong.\n\nhttps://in dico.particle.mephi.ru/event/626/contributions/6221/ LOCATION:Sevastopol Hotel URL:https://indico.particle.mephi.ru/event/626/contributions/6221/ END:VEVENT BEGIN:VEVENT SUMMARY:Limitations of the Diffusion Approximation for GCR Transport DTSTART;VALUE=DATE-TIME:20261030T144500Z DTEND;VALUE=DATE-TIME:20261030T150000Z DTSTAMP;VALUE=DATE-TIME:20261021T104106Z UID:indico-contribution-316-6222@cern.ch DESCRIPTION:Speakers: Vladimir Yurovsky (Lomonsov MSU)\nModern experiments provide a wealth of new data and reveal many new\, still unexplained phen omena. To explain them\, one needs a deep understanding of Galactic cosmic ray (GCR) transport\, which is usually assumed to be diffusive. Many stud ies construct predictive models within different variants of this approach and achieve valuable results in explaining observed GCR spectra. However\ , the validity of this approximation has not been rigorously proven.\n\nIn this work\, we study the microscopic transport of ultra-relativistic part icles. Test-particle simulations are performed for different configuration s of a model magnetic field. From the obtained trajectories\, we extract t he statistical properties of charged-particle reflections from magnetic fi eld inhomogeneities. A data collapse of the joint distribution of reflecti on parameters is obtained using a self-similarity ansatz. The marginal pat h-length distribution exhibits intermediate power-law asymptotic behavior with an exponential cutoff. A strong correlation between particle displace ments and path length also emerges. These results indicate that the diffus ion approximation is applicable only at scales larger than the exponential cutoff\, whereas at smaller scales the transport exhibits strong signatur es of anomalous behavior.\n\nhttps://indico.particle.mephi.ru/event/626/co ntributions/6222/ LOCATION:Sevastopol Hotel URL:https://indico.particle.mephi.ru/event/626/contributions/6222/ END:VEVENT BEGIN:VEVENT SUMMARY:A mass-sensitive criterion for SPHERE-3: dependence on atmospheric and hadronic interaction models DTSTART;VALUE=DATE-TIME:20261030T154500Z DTEND;VALUE=DATE-TIME:20261030T160000Z DTSTAMP;VALUE=DATE-TIME:20261021T104106Z UID:indico-contribution-316-6223@cern.ch DESCRIPTION:Speakers: Vladimir Ivanov (SINP MSU)\nThe SPHERE-3 experiment is being developed to study the mass composition of primary cosmic rays us ing Cherenkov light from extensive air showers reflected from the snow sur face. The lateral distribution of this light carries information about the primary mass\, but its interpretation depends on the atmospheric profile and the hadronic interaction model used in shower simulations.\n\nWe prese nt a physically interpretable mass-sensitive criterion based on ratios of Cherenkov light integrated over radial regions of the reconstructed latera l distribution. A Fisher discriminant combines several radial ratios while retaining their connection to the spatial distribution of light. The appr oach is studied using simulated proton\, nitrogen\, and iron showers\, wit h the telescope response included\, and evaluated through pairwise mass se paration.\n\nBuilding on this analysis\, we outline a comparative study of atmospheric and hadronic interaction models. The planned comparison will examine shifts in the criterion distributions and changes in mass-separati on performance under different simulation assumptions. Applying a criterio n calibrated with one model to samples generated with another will allow i ts transferability to be assessed. This study aims to quantify the sensiti vity of the criterion to modelling choices and to identify the systematic effects that must be considered when using reflected Cherenkov light to in fer cosmic-ray mass composition.\n\nhttps://indico.particle.mephi.ru/event /626/contributions/6223/ LOCATION:Sevastopol Hotel URL:https://indico.particle.mephi.ru/event/626/contributions/6223/ END:VEVENT BEGIN:VEVENT SUMMARY:APPLICATION OF UNIVERSALITY IN CASCADE DEVELOPMENT FOR THE STUDY O F HIGH-ENERGY COSMIC RAYS IN SPACE EXPERIMENTS DTSTART;VALUE=DATE-TIME:20261030T150000Z DTEND;VALUE=DATE-TIME:20261030T151500Z DTSTAMP;VALUE=DATE-TIME:20261021T104106Z UID:indico-contribution-316-6224@cern.ch DESCRIPTION:Speakers: Anastassiya Fedossimova (Institute of Physics and Te chnology)\nMost energy measurement methods used in modern experiments are based on the cascade curve\, i.e.\, the dependence of the cascade size (ty pically expressed as the logarithm of the energy deposition\, log q\, in a given calorimeter layer) on the penetration depth (d) of the cascade into that layer. If the cascade curve reaches its maximum within the calorimet er\, the primary energy can be reconstructed with relatively high accuracy . However\, to measure the cascade maximum\, the calorimeter must have suf ficient thickness\; moreover\, the higher the primary energy\, the thicker the calorimeter needs to be.\nCascade curves exhibit significant fluctuat ions. A cascade may start developing in the first measurement layer\, for example\, or in the tenth layer. Accordingly\, the total energy deposition in the calorimeter for these two cascades will differ substantially. In a ddition\, since the primary energy is determined using the total energy de position\, large fluctuations in the latter lead to large uncertainties in the reconstruction of the primary energy.\n\nIn this work\, a method for reducing fluctuations (LFM) is presented to improve energy reconstruction for data obtained with thin calorimeters. The proposed method is based on the use of so-called correlation curves\, i.e.\, the dependence of the cas cade size (S = log q) on the cascade development rate (R). The cascade dev elopment rate is defined as the difference between cascade sizes at two me asurement levels divided by the calorimeter thickness over which this chan ge occurs:\n\nR = (S₁ − S₂) / (d₁ − d₂)\, where d₁ and d₂ are the penetration depths corresponding to these two measurement layers.\ nThe size–rate curves exhibit minimal fluctuations. They coincide for ca scades that start developing in the first measurement layer and for those that begin in the tenth measurement layer. As a result\, the energy resolu tion achieved with this approach is superior to that obtained using conven tional cascade curves.\n\nThis method is based on the assumption of the un iversality of cascade development for particles with the same energy and c harge. Cascades differ significantly in the parameters of the first intera ction\, which leads to large fluctuations at the initial stage of the casc ade curve.\n\nHowever\, fluctuations become small once a large number of s econdary particles are produced in the cascade.\n\nUsing this method\, the primary energy is reconstructed near the beginning of the cascade develop ment. Thus\, with increasing energy\, there is no need to increase the thi ckness of the calorimeter.\nThe proposed method is universal for a wide ra nge of energies and different nuclei.\n\nhttps://indico.particle.mephi.ru/ event/626/contributions/6224/ LOCATION:Sevastopol Hotel URL:https://indico.particle.mephi.ru/event/626/contributions/6224/ END:VEVENT BEGIN:VEVENT SUMMARY:Recent results on ultra-high-energy cosmic rays from the Telescope Array experiment DTSTART;VALUE=DATE-TIME:20261030T140000Z DTEND;VALUE=DATE-TIME:20261030T141500Z DTSTAMP;VALUE=DATE-TIME:20261021T104106Z UID:indico-contribution-316-6225@cern.ch DESCRIPTION:Speakers: Maria Kudenko (Lomonosov Moscow State University\, T he Institute for Nuclear Research of the Russian Academy of Sciences)\nThe Telescope Array (TA) is the largest cosmic-ray observatory in the Norther n Hemisphere and it is dedicated to studying the origin and properties of cosmic rays over a wide energy range. The experiment consists of two types of detectors: a surface array of scintillation detectors and telescopes d esigned to detect fluorescence and Cherenkov light. Together with its low- energy extension\, TALE\, the Telescope Array covers the energy range from $2\\times 10^{15}$ to $2\\times10^{20}$ eV.\nThe ongoing TAx4 expansion w ill further extend the capabilities of the experiment by increasing its ef fective area by a factor of four\, thereby improving the statistics of the highest-energy cosmic-ray events. This talk will review the current statu s of the TA\, TALE\, and TAx4 projects and summarize recent results from t he Telescope Array Collaboration.\nParticular attention will be given to m easurements of the cosmic-ray mass composition in hybrid mode in the $10^{ 16.5}$–$10^{18.5}$ eV range\, as well as ultra-high-energy photon flux l imits obtained with the use of novel machine-learning approaches. Recent s tudies of correlations between ultra-high-energy cosmic rays and BL Lacert ae-type objects will also be discussed. Finally\, interdisciplinary result s on Terrestrial Gamma-Ray Flashes detected by the TA surface detector wil l be presented.\n\nhttps://indico.particle.mephi.ru/event/626/contribution s/6225/ LOCATION:Sevastopol Hotel URL:https://indico.particle.mephi.ru/event/626/contributions/6225/ END:VEVENT BEGIN:VEVENT SUMMARY:Probing High-Energy Photonuclear Interactions with Muons in Gamma- Ray Air Showers DTSTART;VALUE=DATE-TIME:20261030T160000Z DTEND;VALUE=DATE-TIME:20261030T161500Z DTSTAMP;VALUE=DATE-TIME:20261021T104106Z UID:indico-contribution-316-6226@cern.ch DESCRIPTION:Speakers: Nickolay Martynenko (Lomonosov MSU\, Faculty of Phys ics & Institute for Nuclear Research\, RAS)\nPhotonuclear interactions are the main source of high-energy muons in gamma-ray-induced extensive air s howers (EASs)\, while the corresponding cross section remains poorly const rained at energies relevant for astrophysical gamma rays. We develop an ef ficient framework for propagating uncertainties in the photonuclear cross section to the muon content and photon-selection efficiency of EAS experim ents. We apply it to the Carpet-2 excess of events from the Cygnus region above 300 TeV. Accounting for the source spectrum substantially changes th e expected photon detection efficiency\, while the remaining uncertainty o f the high-energy photonuclear cross section produces an additional sizeab le systematic effect. Their combination removes the apparent tension betwe en the observed excess and the number of muon-poor photon candidates. We a lso show that observations of gamma-ray sources with Carpet-2-like arrays are sensitive to photonuclear interactions in an energy range that is only weakly constrained by laboratory measurements.\n\nThis work was supported by the Russian Science Foundation\, grant 25-12-00333. The speaker acknow ledges a PhD student fellowship from the Theoretical Physics and Mathemati cs Advancement Foundation “BASIS” under contract 24-2-10-39-1.\n\nhttp s://indico.particle.mephi.ru/event/626/contributions/6226/ LOCATION:Sevastopol Hotel URL:https://indico.particle.mephi.ru/event/626/contributions/6226/ END:VEVENT BEGIN:VEVENT SUMMARY:EPOS.LHC-A: first results and impact on muon production in air sho wers DTSTART;VALUE=DATE-TIME:20261030T161500Z DTEND;VALUE=DATE-TIME:20261030T163000Z DTSTAMP;VALUE=DATE-TIME:20261021T104106Z UID:indico-contribution-316-6227@cern.ch DESCRIPTION:Speakers: Roman Nikolaenko ()\nWith great amount of data comin g from collider and fixed-target experiments on all sorts of hadron collis ions\, and with very precise ultra-high energy cosmic ray (UHECR) measurem ents\, many missing pieces of crucial information on the nature of multipa rticle production in quantum chromodynamics (QCD) are now unraveled. The s implified assumptions of old models fail to allow constructing a flexible description needed to satisfy the entire variety of data. The most evident example is the so-called "muon puzzle"\, the excess of $N_{\\mu}$ in UHEC R that remains a challenge to MC calculations even after almost two decade s of studies.\n\nEPOS is a state-of-the-art model that is being developed in a paradigm of a "global approach"\, aiming to provide a universal way o f describing all types of hadronic interactions from $e^+e^-$ to heavy ion collisions\, with its EPOS.LHC-R version being adopted for cosmic ray stu dies.\n\nRecently\, a new string fragmentation model\, ATROPOS\, was inter faced with EPOS.LHC-R\, resulting in a new EPOS.LHC-A version. ATROPOS is a unique approach that considers angular momentum conservation in the proc ess of string fragmentation. This allows to develop a sophisticated treatm ent of heavy resonances production\, along with changes in baryon producti on in hadron collisions. Moreover\, the strict treatment of space-time evo lution of string states is possible with ATROPOS\, which allows a precise connection between string model parameters and the core-corona settings.\n \nIn this talk\, we report the latest developments of ATROPOS model and th e preliminary results of EPOS.LHC-A for hadron production and muon content in EAS.\n\nhttps://indico.particle.mephi.ru/event/626/contributions/6227/ LOCATION:Sevastopol Hotel URL:https://indico.particle.mephi.ru/event/626/contributions/6227/ END:VEVENT BEGIN:VEVENT SUMMARY:Neutrino clusters DTSTART;VALUE=DATE-TIME:20261030T091500Z DTEND;VALUE=DATE-TIME:20261030T093000Z DTSTAMP;VALUE=DATE-TIME:20261021T104106Z UID:indico-contribution-316-6203@cern.ch DESCRIPTION:Speakers: Maxim Dvornikov (Institute of Terrestrial Magnetism\ , Ionosphere and Radiowave Propagation (IZMIRAN))\nThe formation of a neut rino cluster due to an attractive interaction with a hypothetical light sc alar boson is studied. The density distribution of the neutrino gas within the cluster is obtained for various system parameters. It is shown that\, in addition to forming a cluster in space\, the neutrino gas within it ca n form a superfluid condensate. An energy gap equation is derived for such a system\, and the phase transition temperature and coherence length with in the cluster are found. Constraints on the parameters of the interaction leading to neutrino superfluidity are derived. It is found that the super fluid condensate within the cluster consists of relic neutrinos. A neutrin o cluster cooling channel based on the Cherenkov emission of neutrinos in matter is studied if the cluster forms in the early universe. A temperatur e range is obtained for which Cherenkov cooling of the cluster is effectiv e. The possible contribution of neutrino clusters to dark matter is briefl y discussed.\n\nhttps://indico.particle.mephi.ru/event/626/contributions/6 203/ LOCATION:Sevastopol Hotel URL:https://indico.particle.mephi.ru/event/626/contributions/6203/ END:VEVENT BEGIN:VEVENT SUMMARY:Searching for Strangelets and Macro-SQM Candidates from Neutron St ars\, Binary Mergers\, and Gamma-Ray Bursts: Multi-messenger Constraints a nd Direct-Detection Prospects DTSTART;VALUE=DATE-TIME:20261030T093000Z DTEND;VALUE=DATE-TIME:20261030T094500Z DTSTAMP;VALUE=DATE-TIME:20261021T104106Z UID:indico-contribution-316-6204@cern.ch DESCRIPTION:Speakers: Chitta Ranjan Das (Bogoliubov Laboratory of Theoreti cal Physics (BLTP)\, Joint Institute for Nuclear Research (JINR))\nStrange quark matter (SQM) is a compelling candidate for the true ground state of quantum chromodynamics (QCD) at high baryon density. Within the Bodmer-Wi tten-Terazawa hypothesis\, if SQM has a lower energy per baryon than ordin ary hadronic matter\, neutron stars can convert to strange quark stars (SQ Ss). Stable clusters of SQM\, strangelets\, can be produced in dense QCD p hase transitions\, releasing up to $\\sim10^{53}$ erg. Strangelets consist of approximately equal numbers of up\, down\, and strange quarks\; their baryon number $A$ is one third of the total quark number\, and their net e lectric charge is $Z$. Both MIT-bag and Nambu-Jona-Lasinio descriptions pr edict mass-to-charge ratios $m_S/|Z|\\sim30$ to $60$ GeV/$c^2$ for $A\\sim 10^{2}$ to $10^{5}$. A key formation channel is the transition from the tw o-flavor color-superconducting (2SC) phase to the color-flavor-locked (CFL ) phase in dense quark matter. Diquark condensation\, fragmentation of Fer mi surfaces\, and surface emission of quark clusters can produce strangele ts\, while strangelet-anti-strangelet annihilation\, $S\\bar{S}\\to\\gamma \\gamma$\, can generate narrow\, monochromatic very-high-energy (VHE) $\\g amma$-ray lines.\n\nThis work develops a unified framework connecting QCD- motivated strangelet production to observable multi-messenger fluxes. A ph enomenological production-rate model is introduced that balances geometric growth\, $\\dot N(A)\\propto (A/A_{\\rm peak})^{2/3}$\, against exponenti al suppression from multi-fragmentation and coalescence. The framework is applied to three representative astrophysical environments: (i) HESS J1731 $-$347\, a steady SQS candidate with $M=0.77^{+0.20}_{-0.17}M_\\odot$ and $R=10.4^{+0.86}_{-0.78}$ km\, whose 2SC-CFL interface can inject strangele ts into the surrounding supernova remnant\; (ii) GW170817\, the first bina ry neutron-star merger\, where the hadron-to-quark transition in the post- merger remnant can produce a burst-like strangelet flux\; and (iii) GRB 25 0702B\, an ultra-long gamma-ray burst with duration $>25{\,}000$ s and $E_ {\\rm iso}>1.4\\times10^{54}$ erg\, providing an extreme burst-driven chan nel. Constraints from H.E.S.S.\, Fermi-LAT\, MAGIC-II\, and the projected Cherenkov Telescope Array (CTA) are compiled. The baseline scenario lies n ear the CTA sensitivity threshold ($\\sim10^{-13}$ ph cm$^{-2}$ s$^{-1}$ a t 1 TeV)\; the optimistic scenario is already excluded by H.E.S.S.\, while the conservative scenario requires next-generation instruments.\n\nA comp lementary direct-detection program targets macroscopic SQM composites such as nuclearites and Q-balls. Although microscopic strangelets are unlikely to survive interstellar propagation\, these heavier objects possess extre mely large mass-to-charge ratios and high ionization densities\, allowing them to traverse the interstellar medium and penetrate the terrestrial atm osphere. Their passage would produce bright\, continuous high-ionization t racks\, thermal shock fronts\, and slow luminous transits in large-volume detectors. Existing limits from MACRO\, SLIM\, ANTARES\, and IceCube alrea dy constrain parts of the parameter space\, while future facilities includ ing LHAASO\, KM3NeT/ARCA\, SQM-ISS\, and gravitational-wave observatories will provide complementary sensitivity. Combining narrow VHE $\\gamma$-ray line searches with direct macro-SQM detection and multi-messenger follow- up of neutron stars\, mergers\, and GRBs offer a decisive test of the stra nge quark matter hypothesis.\n\nhttps://indico.particle.mephi.ru/event/626 /contributions/6204/ LOCATION:Sevastopol Hotel URL:https://indico.particle.mephi.ru/event/626/contributions/6204/ END:VEVENT BEGIN:VEVENT SUMMARY:The TRGB Luminosity as a Probe of the Axion–Electron Coupling: C onstraints and Theoretical Uncertainties DTSTART;VALUE=DATE-TIME:20261030T094500Z DTEND;VALUE=DATE-TIME:20261030T100000Z DTSTAMP;VALUE=DATE-TIME:20261021T104106Z UID:indico-contribution-316-6205@cern.ch DESCRIPTION:Speakers: Alexey Kudashov (Moscow State University Faculty of Physics)\, Sergey Troitsky (INR\, Moscow)\nRed-giant evolution is sensitiv e to non-standard channels of energy loss and therefore provides a probe o f new physics.\nSuch losses increase the luminosity of the tip of the red- giant branch\n(TRGB)\, enabling constraints on the axion--electron couplin g $g_{ae}$.\nIn this talk\, we present cluster-specific stellar-evolution calculations\nwith MESA for 27 Galactic globular clusters\, including the implementation\nof axion emission and its impact on the predicted TRGB lum inosity.\nParticular attention is given to the assessment of theoretical u ncertainties associated with thermal-neutrino emission\, electron conducti on\, radiative opacity\, nuclear reaction rates\, convection\, and other m odelling assumptions. We examine how these theoretical uncertainties affec t the predicted TRGB luminosities and the resulting constraints on the axi on–electron coupling.\n\nWe briefly outline the joint profile-likelihood analysis used to\ncompare these predictions with TRGB measurements for 24 clusters\,\nafter excluding three hot-flasher systems. Retaining shared\n uncertainties as correlated nuisance parameters\, we obtain\na 95% confide nce-level power-constrained upper limit\nof $g_{ae} \n\nhttps://indico.par ticle.mephi.ru/event/626/contributions/6205/ LOCATION:Sevastopol Hotel URL:https://indico.particle.mephi.ru/event/626/contributions/6205/ END:VEVENT BEGIN:VEVENT SUMMARY:Preliminary Study on Prototype Strings for Baikal-HUNT DTSTART;VALUE=DATE-TIME:20261030T084500Z DTEND;VALUE=DATE-TIME:20261030T090000Z DTSTAMP;VALUE=DATE-TIME:20261021T104106Z UID:indico-contribution-316-6207@cern.ch DESCRIPTION:Speakers: Xiaohao You (Institute of High Energy Physics\, Chin ese Academy of Sciences)\nThe High-energy Underwater Neutrino Telescope (H UNT) project aims to identify astrophysical neutrino sources\, particularl y those associated with ultra-high-energy gamma-ray emission observed by L HAASO. We present the status of its prototype program in Lake Baikal\, cov ering deployment campaigns and preliminary results from 2024 to 2026. Depl oyments progressed from 12 optical modules with 20-inch photomultiplier tu bes in 2024 to 24 complete optical modules in 2025\, followed by a second full prototype string in 2026. These campaigns enabled studies of optical- module response\, depth-dependent counting rates\, and underwater hardware reliability. We report preliminary analyses of muon-like events and joint event studies with Baikal-GVD. Progress in LED timing calibration and opt ical-module positioning is also presented. These results provide technical input and operational experience for further development of Baikal-HUNT a nd support future joint observations with Baikal-GVD.\n\nhttps://indico.pa rticle.mephi.ru/event/626/contributions/6207/ LOCATION:Sevastopol Hotel URL:https://indico.particle.mephi.ru/event/626/contributions/6207/ END:VEVENT BEGIN:VEVENT SUMMARY:Recent results and status of the Baikal-GVD neutrino telescope DTSTART;VALUE=DATE-TIME:20261030T083000Z DTEND;VALUE=DATE-TIME:20261030T084500Z DTSTAMP;VALUE=DATE-TIME:20261021T104106Z UID:indico-contribution-316-6210@cern.ch DESCRIPTION:Speakers: Grigory Safronov (INR RAS)\nHigh-energy astrophysica l neutrinos can provide a probe of hadronic processes at their production site constraining models of the most energetic cosmic ray sources. The dif fuse astrophysical neutrino flux was discovered by the IceCube experiment more than a decade ago but still remains largely unexplored. After the dep loyment campaign in 2026\, the Baikal-GVD neutrino telescope has reached t he detection volume of 0.8 km3 and it is planned to further expand it to 1 km3 in the next two-three years. Meanwhile the detector joins the study of the origins of high-energy cosmic neutrinos with the data accumulated at the construction phase. In present report we discuss the status and recent physics results of Baikal-GVD among them are the measurement of the diffu se astrophysical neutrino flux and neutrino source searches.\n\nhttps://in dico.particle.mephi.ru/event/626/contributions/6210/ LOCATION:Sevastopol Hotel URL:https://indico.particle.mephi.ru/event/626/contributions/6210/ END:VEVENT BEGIN:VEVENT SUMMARY:Cosmic rays from 1 GeV to 100 EeV due to star formation processes? DTSTART;VALUE=DATE-TIME:20261030T100000Z DTEND;VALUE=DATE-TIME:20261030T101500Z DTSTAMP;VALUE=DATE-TIME:20261021T104106Z UID:indico-contribution-316-6211@cern.ch DESCRIPTION:Speakers: Timur Dzhatdoev (INR RAS)\, Anatolii Semenov (INR)\n Star formation processes are very important in the Universe. In particular \, the formation of massive stars results in supernova explosions with sub sequent acceleration of cosmic rays (CR) in supernova remnants (SNRs). We show that the currently-available elemental spectra of protons\, Helium\, CNO group nuclei\, and Iron in the energy range from 40 GeV to 100--500 Pe V are well described with two separate populations of Galactic SNRs. We pr opose a scenario where the extragalactic CR component is produced by a thi rd distinct population of SNRs\; these SNRs probably have sub-relativistic speeds of shock waves and/or are the remnants of powerful hypernovae. The n we discuss a possibility that these three SNR populations dominate the e ntire observable spectrum of CR protons and nuclei spanning from 1 GeV to 100 EeV. Some details are available in astro-ph/2606.02748 (submitted to M NRAS).\n\nhttps://indico.particle.mephi.ru/event/626/contributions/6211/ LOCATION:Sevastopol Hotel URL:https://indico.particle.mephi.ru/event/626/contributions/6211/ END:VEVENT BEGIN:VEVENT SUMMARY:Dark-matter relay for ultra-high-energy cosmic rays DTSTART;VALUE=DATE-TIME:20261030T101500Z DTEND;VALUE=DATE-TIME:20261030T103000Z DTSTAMP;VALUE=DATE-TIME:20261021T104106Z UID:indico-contribution-316-6213@cern.ch DESCRIPTION:Speakers: Mikhail Sekretov (INR\, MSU)\nAstrophysical sources of ultra-high-energy cosmic rays (UHECRs) remain unidentified\, and no nea rby cosmic accelerators are established even for the highest-energy events . In addition\, puzzling correlations of a fraction of UHECR flux with dis tant blazars were found by HiRes and\, recently\, Telescope Array experime nts. Here we propose that dark matter can provide a mechanism to effective ly transfer UHECRs from distant sources: dark-matter particles are boosted by UHECRs near the source and pass their momentum to baryons close to the observer. The probability of this relay is not negligible because of the growth of dark-matter–baryon cross section with energy. We demonstrate t hat the effect is observable for the fermionic dark matter of the mass $m_ \\mathrm{DM} \\sim 25 \\\, \\mathrm{MeV}$ and discuss possible observation al signatures of this mechanism.\n\nhttps://indico.particle.mephi.ru/event /626/contributions/6213/ LOCATION:Sevastopol Hotel URL:https://indico.particle.mephi.ru/event/626/contributions/6213/ END:VEVENT BEGIN:VEVENT SUMMARY:High energy Galactic neutrinos in a local PeVatron scenario DTSTART;VALUE=DATE-TIME:20261030T090000Z DTEND;VALUE=DATE-TIME:20261030T091500Z DTSTAMP;VALUE=DATE-TIME:20261021T104106Z UID:indico-contribution-316-6215@cern.ch DESCRIPTION:Speakers: Simon Sotirov (MSU\, INR RAS)\nWe investigate and ma ke theoretical estimates for the neutrino flux above 150 TeV in a scenario with a nearby source in the Cygnus region\, the existence of which is mot ivated by the LHAASO gamma-ray bubble observations. By combining a state-o f-the-art model of galactic cosmic rays with the contribution from a local source within the framework of a two-zone diffusion model\, we investigat e the neutrino signal for anisotropy.\n\nhttps://indico.particle.mephi.ru/ event/626/contributions/6215/ LOCATION:Sevastopol Hotel URL:https://indico.particle.mephi.ru/event/626/contributions/6215/ END:VEVENT BEGIN:VEVENT SUMMARY:THE INFLUENCE OF RELATIVISTIC EFFECTS ON THE PARAMETERS OF NEUTRON STAR MODELS DTSTART;VALUE=DATE-TIME:20261029T070000Z DTEND;VALUE=DATE-TIME:20261029T071500Z DTSTAMP;VALUE=DATE-TIME:20261021T104106Z UID:indico-contribution-316-6193@cern.ch DESCRIPTION:Speakers: Alina Shmakova (Astrakhan State University named V. N. Tatishchev)\nAbstract: The paper theoretically investigates the equilib rium structure of neutron stars consisting of degenerate relativistic neut ron gas\, based on the equation of radial mass distribution. The thermodyn amic properties of a relativistic Fermi gas are studied\, and a relationsh ip between the compressibility coefficient and the particle concentration is established without taking nuclear forces into account. The mass distri bution equation is numerically solved for the pulsar PSR J0740+6620\, and its radius\, as well as the radial distributions of density\, pressure\, a nd Fermi energy\, are determined. A comparison of relativistic and non‑r elativistic models was carried out\, showing that taking relativistic effe cts into account leads to a denser star with a smaller radius. Based on nu merical calculations\, the Oppenheimer–Volkoff limit was estimated.\n\nK eywords: neutron star\, degenerate relativistic neutron gas\, radial distr ibution of the star’s mass.\n\nNeutron stars are giant cores consisting of degenerate neutron gas\, primarily bound by gravitational forces. The d ensity distribution of stellar matter is examined using the example of the pulsar PSR J0740+6620\, whose mass is (2.08  0.07) times the mass of t he Sun [1].\nThe radial mass distribution function m(r) of an adiabatic st ar in the absence of rotation obeys the equation [2]:\n m^{″}-\\frac{2} {r}m^{\\prime }+\\frac{G}{4\\pi }\\kappa {\\left(\\frac{m^{\\prime }}{r^{2 }}\\right)}^{2}m=0\, (1)\nwhere κ is the compressibility of the substa nce\, G is the gravitational constant. It satisfies the boundary condition s: m(0)=0 and m(R)=M \, where M is the mass of the star\, and R is its rad ius. The compressibility of a degenerate relativistic neutron gas is expre ssed as [3]:\n \\kappa =\\frac{9}{\\pi }\\cdot \\frac{(ch)^{3}}{8E_{0}^{4 }}\\cdot \\frac{(1+x^{2})^{1/2}}{x^{5}}\, где x=\\frac{hc}{2E_{0}}{\\le ft(\\frac{3n}{\\pi }\\right)}^{1/3}. (2)\nHere\, n is the particle concen tration\; E0 is the rest energy of the neutron\; h is Planck’s constant\ ; c is the speed of light. In the non‑relativistic approximation x\n\nht tps://indico.particle.mephi.ru/event/626/contributions/6193/ LOCATION:Sevastopol Hotel URL:https://indico.particle.mephi.ru/event/626/contributions/6193/ END:VEVENT BEGIN:VEVENT SUMMARY:Dynamics of nuclear reactions in the outer crust of transiently ac creting neutron stars DTSTART;VALUE=DATE-TIME:20261029T061500Z DTEND;VALUE=DATE-TIME:20261029T063000Z DTSTAMP;VALUE=DATE-TIME:20261021T104106Z UID:indico-contribution-316-6186@cern.ch DESCRIPTION:Speakers: Nikita Zemlyakov (Ioffe Institute)\nSome neutron sta rs are located in low-mass X-ray binaries (LMXBs)\, i.e. have low-mass com panions. In these systems\, matter from the companion is transferred via R oche-lobe overflow and accretes onto the neutron star. The accretion proce ss can be either transient or persistent. During accretion\, the previousl y accreted material is compressed under the weight of newly accreted matte r. In the outer crust\, the pressure is primarily determined by degenerate electrons\; consequently\, this compression leads to an increase in the e lectron chemical potential. Such an increase can drive electron capture re actions out of equilibrium. Previous studies investigating the nuclear evo lution of accreted matter in the neutron star crust can be divided into tw o groups: (1) those that consider variable accretion rates but assume elec tron capture reactions occur instantaneously\; and (2) those that account for finite reaction rates but assume a steady (stationary) accretion rate. \n\nA recent study [1] examined non‑stationary accretion while accountin g for finite electron capture rates. However\, the capture rate was comput ed using the zero‑temperature approximation. Under this approximation\, the reaction rate is exactly zero below the threshold density and increase s sharply above it. Using this approach\, the authors of [1] demonstrated that the crust structure is non‑stationary. During an accretion episode\ , the composition of the outer crust evolves away from beta equilibrium du e to the accumulation of nuclei above the threshold. During a quiescent st ate\, these accumulated nuclei are burnt out\, which results in a nearly b eta‑equilibrium composition restored before the next accretion episode b egins. This leads to a cyclical pattern in the crust’s composition. \n\n In this work\, we investigate the dynamics of nuclear reactions under cond itions of non‑stationary accretion\, incorporating finite‑temperature reaction rates. We show that this approach substantially alters the physic al picture. Due to thermal excitations\, electron capture reactions become effective even below the nominal threshold density. At the same time\, th e reverse reaction is suppressed: it is inhibited by a subsequent electron capture on the daughter nuclei. This second capture is superthreshold bec ause of nuclear pairing effects – the daughter nucleus is odd‑odd\, so the threshold density is low. Furthermore\, the dependence of the reactio n rates on density becomes less pronounced. Consequently\, the composition of the outer crust evolves more slowly compared to the model presented in [1]. As a result\, the composition at the onset of an accretion episode d epends on the long‑term accretion history of the system. In particular\, this effect can lead to a substantial release of energy during a strong a ccretion episode as a result of burning of nuclei that accumulated in the crust during earlier accretion. \n\nThe work is supported by Russian Scien ce Foundation (grant No. 22-12-00048-P).\n\n[1] Suleiman\, L.\, Zdunik\, J . L.\, & Haensel\, P. (2024). Layers of electron captures in the crust of accreting neutron stars. A&A\, 690\, A301.\n\nhttps://indico.particle.meph i.ru/event/626/contributions/6186/ LOCATION:Sevastopol Hotel URL:https://indico.particle.mephi.ru/event/626/contributions/6186/ END:VEVENT BEGIN:VEVENT SUMMARY:Quantum Mechanical Numerical Model of XHe–Nucleus Interaction an d Direct Dark Matter Searches DTSTART;VALUE=DATE-TIME:20261029T071500Z DTEND;VALUE=DATE-TIME:20261029T073000Z DTSTAMP;VALUE=DATE-TIME:20261021T104106Z UID:indico-contribution-316-6187@cern.ch DESCRIPTION:Speakers: Maxim Khlopov (Virtual Institute of Astroparticle Ph ysics)\nWhile Standard Model extensions such as Supersymmetry have long pr ovided promising candidates\, the absence of supersymmetric particle signa ls at the LHC and contradictory results from direct detection experiments motivate exploration of alternative scenarios. The hypothesis of composite dark atoms — electrically neutral atom-like bound states formed by stab le doubly negatively charged particles with primordial helium nuclei — o ffers a promising framework to address the challenges in direct dark matte r detection. We present self-consistent quantum-mechanical numerical model for describing the three-body interaction between X-helium (XHe) dark ato ms and nuclei of ordinary matter\, bridging cosmoparticle physics\, nuclea r physics\, and experimental dark matter searches. The methodology incorpo rates nuclear\, Coulomb\, centrifugal\, and Stark interaction potentials\, enabling precise reconstruction of the effective interaction potential fo r XHe with sodium and iodine nuclei. Our results reveal a crucial selectiv ity: while the effective potential for sodium supports the radiative captu re of the sodium nucleus by the dark atom into a single low-energy bound s tate with binding energy in the 1–6 keV range\, consistent with the DAMA /LIBRA annual modulation signal\, the corresponding radiative capture rate s for iodine are substantially suppressed. This selectivity of modulation signal generation in the detector depending on the target nucleus naturall y explains the observed signal in NaI detectors and its absence in experim ents using heavier target nuclei\, while satisfying experimental constrain ts on high-energy gamma emission. The results obtained validate the dark a tom hypothesis as a coherent resolution to long-standing puzzles in dark m atter direct searches. The developed model establishes a framework for int erpreting experimental results and for future investigations of composite dark matter candidates.\n\nhttps://indico.particle.mephi.ru/event/626/cont ributions/6187/ LOCATION:Sevastopol Hotel URL:https://indico.particle.mephi.ru/event/626/contributions/6187/ END:VEVENT BEGIN:VEVENT SUMMARY:A FISSION FLASH IN THE INNER CRUST OF AN EXPLODING LOW-MASS NEUTRO N STAR DTSTART;VALUE=DATE-TIME:20261029T063000Z DTEND;VALUE=DATE-TIME:20261029T064500Z DTSTAMP;VALUE=DATE-TIME:20261021T104106Z UID:indico-contribution-316-6189@cern.ch DESCRIPTION:Speakers: Anton Ignatovskiy (MIPT\, NRC "Kurchatov Institute") \nAmong the scenarios for the evolution of various astrophysical objects i n which the conditions necessary for the r‑process to occur can be reali zed\, the process of neutron star mergers in a close binary system is curr ently considered the main one [1]. This scenario largely depends on the ma sses of the objects included in the system and can develop in different wa ys: 1) If neutron stars have approximately the same mass\, a merger occurs \, accompanied by the ejection of neutron‑rich matter in the equatorial plane and in the wind from the hot\, massive neutron star [2]\; 2) If the masses of the neutron stars differ significantly\, the evolution of the ne utron star system follows a stripping scenario [3]\, in which\, in particu lar\, the nucleosynthesis of heavy elements proceeds differently [4\,5].\n The first ideas about the merger of a neutron star (NS) and a black hole a ssociated with short gamma-ray bursts (GRB) were put forward by Lattimer a nd Schramm [6]. The scenario of the merger of two neutron stars was deve loped by Clark and Eardley [3]. In the last paper not only the merging of two neutron stars was discussed\, but also proposed a stripping scenario i nvolving the loss of mass by a minimum mass star.\nIn both scenarios\, two neutron stars orbiting each other must come closer due to the loss of ang ular momentum caused by the emission of gravitational waves. What is the d ifference between the merger and tidal disruption mechanisms? The merger m echanism is as follows: having approached each other to a sufficient dista nce\, the neutron stars merge into a single object — a black hole or a r apidly rotating neutron star — over several orbits. At the same time\, p art of the matter may be ejected from the system due to tidal interaction. Furthermore\, due to the extreme acceleration of the rotation of the matt er and its heating\, a highly collimated ejection of matter can form — a jet — and part of the matter of the merged neutron star can evaporate i n the form of a wind. This picture of neutron star mergers is currently ge nerally accepted\, although many of its details remain unclear.\nThe funda mental difference between the stripping mechanism and a rapid merger lies in the prolonged (many orbits of the binary system) transfer of matter fro m one star to the other. Note that for this scenario to be realized\, a su fficient asymmetry in the masses of the components of the binary system is required. As the neutron stars approaches\, the component with the smalle r mass first fills its Roche lobe\, since it has a larger radius\, and beg ins to transfer mass to the more massive companion through the inner Lagra nge point. The asymmetry of the system increases\, and the distance betwee n the stars increases due to the approximate conservation of the system’ s angular momentum. However\, the transfer does not stop (it is stable) du e to the loss of angular momentum through the emission of gravitational wa ves and the increase in the radius of the NS with the smaller mass. \nAs a result of the exchange\, the mass of the heavier star (M1) increases\, w hile its radius remains approximately constant or decreases\, and the mass of the lighter NS (M2) decreases while its radius increases. When M2 reac hes the value corresponding to the minimum possible mass of the NS (about 0.1 solar masses)\, an explosion occurs\, which leads to the destruction o f the low‑mass NS.\nThis report examines the nucleosynthesis of heavy nu clei under the influence of neutrons (the r‑process) in the inner crust of a low‑mass neutron star (LMSN)\, which loses mass due to the transfer of matter onto a more massive companion neutron star (the stripping scena rio) and explodes upon reaching a hydrodynamically unstable configuration [7]. \nIt has been shown that the schock wave generated during the destru ction of the MMNZ heats the outer shell of the inner core to high temperat ures\, and the r‑process transforms into explosive nucleosynthesis. Sinc e the cross‑sections of induced fission increase by orders of magnitude when the temperature rises to values of T9>5\, and given the persistently high neutron density\, an instantaneous (t~3–5 ms) fission flash of the actinides formed in the r‑process occurs. The composition of the resulti ng fission product nuclei largely depends on the model of the mass distrib ution of fission products and represents a new initial composition for the r‑process\, which resumes after further expansion of the matter and a d rop in temperature.\nThe work was carried out as part of fulfilling the st ate assignment of the National Research Center “Kurchatov Institute”.\ nLITERATURE\n1. J. J. Cowan\, et al. // Rev. Mod. Phys. 2021. V. 93. id. 1 5002.\n2. S. Rosswog\, Philosophical Transactions of the Royal Society A. 2013\, V. 371\, № 1992\, 20120272.\n3. J. P. A. Clark and D. M. Eardley // Astrophys. J. 1977. V. 215. P. 311.\n4. I.V. Panov\, A.V. Yudin // Astr onomy Letters. 2020. V. 46. P. 518.\n5. A. Yudin\, N. Kramarev\, I. Panov\ , A. Ignatovskiy // Particles. 2023. V. 6. P. 784. \n6. J.M. Lattimer\, D. N. Schramm // Astrophys. Lett. 1974. V. 192. P. 145.\n7. S. I. Blinnikov\ , D. K. Nadyozhin\, N. I. Kramarev\, A. V. Yudin // Astronomy Reports. 202 1. V. 65. P. 385.\n\nhttps://indico.particle.mephi.ru/event/626/contributi ons/6189/ LOCATION:Sevastopol Hotel URL:https://indico.particle.mephi.ru/event/626/contributions/6189/ END:VEVENT BEGIN:VEVENT SUMMARY:Axion-like particle emission from type Ia supernovae DTSTART;VALUE=DATE-TIME:20261029T064500Z DTEND;VALUE=DATE-TIME:20261029T070000Z DTSTAMP;VALUE=DATE-TIME:20261021T104106Z UID:indico-contribution-316-6190@cern.ch DESCRIPTION:Speakers: Daniil Davydov (INR\, MSU)\nAxion-like particles (AL Ps) are a class of hypothetical bosons beyond the standard model of partic le physis\, which are\nvery weakly-interacting and long- lived. Since many ALPs may be produced in hot plasma in supernovae (SNe)\, a nearby\nSNe Ia can be used as a probe of ALPs. It is desirable to predict the ALP emissi on from SNe Ia to discuss a possible\nconstraint that can be obtained from the event. ALPs may convert into photons and back in the magnetic field i n the\nintergalactic space and galaxies. It is hence possible to constrain the ALP parameters by γ-ray observations of a nearby\nastronomical objec t which emits a lot of ALPs. Here\, we calculate the ALP emission from typ e Ia SNe and take into the\naccount the light range of ALPs mass. Using th e SN Ia model\, we consider the issue of detection a photon flash from\nSN e Ia\n\nhttps://indico.particle.mephi.ru/event/626/contributions/6190/ LOCATION:Sevastopol Hotel URL:https://indico.particle.mephi.ru/event/626/contributions/6190/ END:VEVENT BEGIN:VEVENT SUMMARY:Jet Activity in the Central Super Massive Black Hole of the Milky Way in 4th and 14th centuries and millennial periods of the climate change DTSTART;VALUE=DATE-TIME:20261029T074500Z DTEND;VALUE=DATE-TIME:20261029T080000Z DTSTAMP;VALUE=DATE-TIME:20261021T104106Z UID:indico-contribution-316-6191@cern.ch DESCRIPTION:Speakers: Olga Piskounova (FIAN)\nThis paper discusses the hi storical evidence for the light jets from the central Super Massive Black Hole of Galaxy in the 4th and 14th centuries. We suggest that the appariti ons of a "lightening cross" recorded in 312\, 351\, 1317 and 1377 years we re caused by the line of two jets beamed back-to-back from the center of M ilky Way (MW)\, which is crossing the visible projection of the Galaxy dis k. All historical accounts give precise time and geographical locations\, where from X-crosses was seen: in the vicinity of Rome\, in Jerusalem\, in Tver' (the vicinity of Moscow) and in night sky over Moscow\, respectivel y). The positions of the Sun (or the Moon) were also mentioned in the Midd le Age manuscripts. These positions coincide with the location of the MW c enter on the sky map in these specific places and dates\, as it is shown w ith the help of Wolfram Astronomy visualization instruments.As it was rece ntly found from media\, another memorial for MW jet of 4th century might b e geoglyph on the rocky cliff\, which is situated in shores of Paracas Bay in Peru. We suggest that the gap between jet activity events is about tho usand years. The X cross in the sky was mentioned by Plato in {\\it Timaeu s}\, but he can not be eyewitness and could only take this from the narrat ives of older ancient sages. The X cross pictures are multiply stamped on Roman coins. The processes in Galaxy are often periodic because of multipl e orbital movements\, so we should consider the millennium periods in the climate changes as well. There are specific variations that are repeated e very thousand years. Variations in temperatures that are described in this work can be explained with reactions of Sun on the waves of astropaticles from Galaxy center: HE protons\, light mass particles\, neutral Baryonium Dark Matter (BDM) or absence of any radiation.The most dangerous periods of BDM conglomerates arrivals\, which suppressed the Sun activity\, happen ed at approximately 6th and 16th centuries and were named Little Ice Ages. Now\, due to our hypothesis\, the Earth is living at the same hottest per iod as it were in the beginning of 1st or 11th centuries. But the continua tion of periods should not be repeated precisely\, because the QCD interac tions are the subject of strong fluctuations.\n\nhttps://indico.particle.m ephi.ru/event/626/contributions/6191/ LOCATION:Sevastopol Hotel URL:https://indico.particle.mephi.ru/event/626/contributions/6191/ END:VEVENT BEGIN:VEVENT SUMMARY:Efficiency of photon production in a strongly magnetized medium DTSTART;VALUE=DATE-TIME:20261029T073000Z DTEND;VALUE=DATE-TIME:20261029T074500Z DTSTAMP;VALUE=DATE-TIME:20261021T104106Z UID:indico-contribution-316-6192@cern.ch DESCRIPTION:Speakers: Dmitry Rumyantsev ()\nThe process of double Compton scattering\, $e \\gamma \\to e \\gamma \\gamma$\, in the presence of a str ongly magnetized\, both charge-asymmetric and charge-symmetric electron pl asma is considered. The amplitude of the process is written out and\nthe s election rules for photon polarizations are found.By solving the kinetic e quation\, an estimate of the efficiency of polarized photon production is obtained.\n\nhttps://indico.particle.mephi.ru/event/626/contributions/6192 / LOCATION:Sevastopol Hotel URL:https://indico.particle.mephi.ru/event/626/contributions/6192/ END:VEVENT BEGIN:VEVENT SUMMARY:Two anomalous components of gamma-rays from GRB 221009A DTSTART;VALUE=DATE-TIME:20261029T060000Z DTEND;VALUE=DATE-TIME:20261029T061500Z DTSTAMP;VALUE=DATE-TIME:20261021T104106Z UID:indico-contribution-316-6195@cern.ch DESCRIPTION:Speakers: Timur Dzhatdoev (INR RAS)\nGRB 221009A was a remarka ble gamma-ray burst\; it is sometimes referred to as “the brightest of a ll time” (BOAT). In this talk we consider two peculiar components of obs ervable gamma-rays from GRB 221009A: 1) a high energy “echo” of the GR B\nprompt emission phase produced by neutrons from photohadronic interacti ons inside the fireball with subsequent interaction of these neutrons with the material of the star forming region (SFR) and 2) external Compton (EC ) radiation due to the scattering of the accelerated electrons on the radi ation reflected from the SFR material. We show that both components are po tentially observable. In addition\, we discuss the shape of the primary (i ntrinsic) gamma-ray spectrum of GRB 221009A and the nature of the 300 TeV gamma-ray-like event detected by the Carpet-3 array in temporal and angula r coincidence with GRB 221009A. Some details are available in astro-ph/260 4.10378.\n\nhttps://indico.particle.mephi.ru/event/626/contributions/6195/ LOCATION:Sevastopol Hotel URL:https://indico.particle.mephi.ru/event/626/contributions/6195/ END:VEVENT END:VCALENDAR