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SUMMARY:GRISP Scientific Instrument Suite for High-Energy Solar Radiation 
 Studies
and Monitoring aboard the ARKA Space Complex
DTSTART;VALUE=DATE-TIME:20261030T133000Z
DTEND;VALUE=DATE-TIME:20261030T133500Z
DTSTAMP;VALUE=DATE-TIME:20261029T152106Z
UID:indico-contribution-6485@cern.ch
DESCRIPTION:Speakers: Mikhail Korotkov (National Research Nuclear Universi
 ty MEPhI (Moscow Engineering Physics Institute))\nStudies of solar activit
 y and prediction of the effects of coronal mass ejections and high-energy 
 radiation from solar flares on near-Earth space and the biosphere are amon
 g the major objectives of solar and solar–terrestrial physics. The GRISP
  (Gamma -\, X-radianion and Solar Protons) instrument suite is designed to
  measure the energy and time distributions and intensities of electromagne
 tic radiation from solar flares over the energy range from 50 keV to 200 M
 eV\, and to detect solar protons with energies above 20 MeV and neutrons w
 ith energies above 30 MeV. CeBr₃ and CsI(Tl) inorganic scintillation det
 ectors measure X-ray and gamma-ray radiation in the energy ranges 0.05–1
 5 MeV and 0.2–200 MeV\, respectively. Neutrons with energies above 30 Me
 V are additionally identified in the CsI(Tl) detector from the scintillati
 on pulse shape. Solar protons are detected by a multilayer detector compos
 ed of polystyrene scintillators. The proton energy is determined from the 
 particle range and energy losses in the individual layers. This technique 
 enables reconstruction of the energy spectrum and measurement of the flux 
 intensity of solar protons above 20 MeV\, as well as studies of their temp
 oral behaviour. Simultaneous measurements in these energy ranges are impor
 tant for understanding particle-acceleration models in solar flares and fo
 r identifying precursor signatures relevant to space-weather forecasting\,
  in particular solar proton events (SPEs) and ground-level enhancements (G
 LEs). The energy resolution and detection efficiency of GRISP enable measu
 rements of line and gamma-ray emission from X-class solar flares\, as well
  as solar-proton fluxes above 100 MeV at intensities exceeding 1 particle 
 cm⁻² s⁻¹ sr⁻¹ (pfu)\, while the detection system supports a maxim
 um counting rate of 10⁵ s⁻¹.\n\nhttps://indico.particle.mephi.ru/even
 t/626/contributions/6485/
LOCATION: Hall
URL:https://indico.particle.mephi.ru/event/626/contributions/6485/
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