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Radiation conditions during the GAMMA-400 observations: orbit, doses and particles fluxes

Radiation conditions during the GAMMA-400 observations: orbit, doses and particles fluxes. GAMMA-400 at the NAVIGATOR-2` satellite platform. The evolution of the perigee and apogee altitudes of the working orbit with time. Radiation conditions

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Radiation conditions during the GAMMA-400 observations: orbit, doses and particles fluxes

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  1. Radiation conditions during theGAMMA-400 observations: orbit, doses and particles fluxes

  2. GAMMA-400 at the NAVIGATOR-2` satellite platform

  3. The evolution of the perigee and apogee altitudes of the working orbit with time

  4. Radiation conditions • ESA's Space Environment Information Systemsoftware • (developed by theBelgian Institute for Space Aeronomy under ESA contracts) • CREME96 software • (созданная в Исследовательской лаборатории ВМФ США) • Accumulated doses software SHIELDOSE2 • We took into account charged particles interaction with Earth magnetosphere and solar activity

  5. Modeling of the dependence of altitude on the satellite coordinates during satellite moving (perigee ~500 km, apogee~300000 km, inclination 51,8 in the beginning period)

  6. Modeling of the dependence of altitude on the satellite coordinates during satellite moving in the Earth magnetosphere (perigee ~500 km, apogee~300000 km, inclination 51,8 in the beginning period)

  7. The maximum intensity particles sources on the satellite orbits: Earth radiation belts (ERB) Solar cosmic rays (mainly solar flares) Galactic cosmic rays.

  8. Solar cosmic rays • Solar cosmic rays– accelerated during solar flares charged particles : • protons Е from0.1 MeVup to 2.104MeV (the maim part) , • also: • -particles, • nuclei withZ>2 (up to28Ni) andЕ from0.1 up to100 MeV/nucleon, • electrons with E>0.03 MeV, • neutrons. • SCL max flux during solar activity max. • semi-empirical SINP MSU model– based on SCL particles characteristic definite regularities (GOST-R-25645-2001), • and modelISO TS-15390-2004:solar active region ejected particles fluxes + fluxes of accelerated particles by solar active region generated blast wave later at 0.5÷1.5 daysafter high energy particles (p+with Е < 30MeV)).

  9. Galactic cosmic rays (GCR) protons(>90%), nuclei 4He (~7%), more heavy nuclei (~1%) electrons(~1%) GCR flux vary depends of solar activity level because of particles scattered by Earth magnetosphere. Flux will be minimal during solar maximum and spectra are different in the solar maximum and minimum high apogee orbit – mainly influence of GCR in the background (outside ERB and solar wind shock wave and when solar flares absent)

  10. the scheme of the Earth magnetic field

  11. influence of solar wind to Earth magnetosphere

  12. The intensity of the ERB particles influence =f(satellite position on the orbit).

  13. The rigidity thresholds for various L

  14. The example: CGRO/BATSE background low altitude orbit data residial model residial

  15. low altitude orbit high altitude orbit

  16. The scheme of Earth magnetic field and THEMIS data

  17. The Earth magnetic field and solar wind on THEMIS and GEOTAIL data

  18. T,min the duration of the times of satellite passing through ERB t, days

  19. The time intervals of the satellite passing of the ERB

  20. flux, cm-2s-1 The dependence of ERB protons fluxes (cm-2s-1)in the band Е>100 keVon the geomagnetic latitude L for 30 days of flight

  21. cm-2s-1MeV-1 energy, MeV averaged spectrum for GCR protons (m-2 c-1MeV-1vs energy (MeV)) on the working part of high apogee orbit

  22. cm-2s-1MeV-1 energy, MeV averaged spectra for several GCR nuclei (m-2 c-1MeV-1vs energy (MeV))

  23. flux, cm-2s-1sr--1 flux, cm-2s-1sr--1 time, s time, s flux, cm-2s-1sr--1 The time variation of protons flux (sm-2 s-1 sr-1) at 3 subsequential segments of high apogee orbit for energy E>300MeV (modeling) time, s

  24. flux, cm-2s-1sr--1 flux, cm-2s-1sr--1 time, s time, s flux, cm-2s-1sr--1 The time variation of protons flux (sm-2 s-1 sr-1) at 3 subsequential segments of high apogee orbit or energy E>500MeV (modeling) time, s

  25. flux, cm-2s-1sr--1 time, s The time variation of protons flux (sm-2 s-1 sr-1) at working region of high apogee orbit (outside Earth magnetosphere) (modeling) flux, cm-2s-1sr--1 time, s

  26. altitude, km flux, cm-2s-1sr--1 He >10 GeV He >1 GeV He >512 MeV He >100 MeV р >10 GeV time, s altitude, km The time and altitude variation of 4He flux (sm-2 s-1 sr-1) at working region of high apogee orbit (outside Earth magnetosphere) (modeling) He >10 GeV He >1 GeV He >512 MeV He >100 MeV р >10 GeV flux, cm-2s-1sr--1 time, s

  27. flux, cm-2s-1sr--1 С > 512 MeV С > 100MeV altitude, km С > 1 GeV С > 10 GeV О > 100 MeV О > 512 MeV О > 1 GeV О > 10 GeV altitude, km flux, cm-2s-1sr--1 time, s С > 512 MeV С > 100MeV The time and altitude variation of 12C and16О flux (sm-2 s-1 sr-1) at working region of high apogee orbit (outside Earth magnetosphere) (modeling) С > 1 GeV С > 10 GeV О > 100 MeV О > 512 MeV О > 1 GeV О > 10 GeV time, s

  28. The preliminary estimations of averaged fluxes of GCR protons and helium nuclei

  29. THEMIS, 2011

  30. Ulysis

  31. GEOTAIL, 1994 #302 #225

  32. The estimations of averaged background fluxes of protons and electrons in the experiments GEOTAIL andUlysis, cm-2s-1sr-1 *Now these data presented without efficiency of registration

  33. conclusions • Very complex background models should be constructed for low altitude orbits for processes with duration more than tens of minutes because of short period (~90 min) • High altitude orbits (for example with perigee of 500 km and apogee of 300000km) are more preferable for long durations events observations • For high altitude orbit the estimated total accumulated dose in Si will be 15 krad (larger than low ones) and equivalent 2-4 mm Al shield should be used for electronic components in dependence of their radiation hardness. • Anticoincidence shield count rates strongly depend on threshold will very low to provide high efficiency of charged particles registration. The estimations were made using GEOTAIL and Ulysis data and gives values of 2 particles per cm-2s-1for protons with energy E>0.3 MeV inside the outer magnetosphere and 100 particles per cm-2s-1 in the blast wave boundary outside the outer magnetosphere • The detectors background charged particles count rates were estimated using SPENVIS software packet and gives values of 2,710-1cm-2s-1sr-1for protons with energy E>100 MeV in the telescope working area

  34. Thank you for attention !!!!

  35. The dependence of protons flux (sm-2 s-1 sr-1) on L for high apogee orbit (modeling)

  36. Ulysis

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