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 ESA's Space Environment Information System software (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

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)

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)

The maximum intensity particles sources on the satellite orbits: Earth radiation belts (ERB) Solar cosmic rays (mainly solar flares) Galactic cosmic rays. Depend on altitude and inclination of orbit, solar activity level 2 types of ERB: internal – mostly protons with Е up to several hundreds MeV, external – electrons with Е up to several tens of MeV The influence of ERB particles observed at the all types of orbits up to L~ 20 depending on the solar activity level. The maximum of such influence observed during satellite pass through SAA and polar regions

Solar cosmic rays Solar cosmic rays – accelerated during solar flares charged particles : protons Е from 0.1 MeV up to 2.104 MeV (the maim part) , also: -particles, nuclei with Z>2 (up to 28Ni) and Е from 0.1 up to 100 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 model ISO 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 days after high energy particles (p+ with Е < 30MeV)).

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)

the scheme of the Earth magnetic field

influence of solar wind to Earth magnetosphere

The integral protons count rate maps in the band Е>10 MeV (AP-8 MAX model)

The integral electrons count rate maps in the band Е>1 MeV (AE-8 MAX model) The intensity of the ERB particles influence =f(satellite position on the orbit).

Direction averaged integral electrons fluxes on the geomagnetic equator at the various L in the AE-8 MAX model

Direction averaged integral protons fluxes on the geomagnetic equator at the various L in the AP-8 MAX model

The rigidity thresholds for various L

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

low altitude orbit high altitude orbit

The scheme of Earth magnetic field and THEMIS data

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

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

The time intervals of the satellite passing of the ERB № orbit perigee, km apogee, km Вtime of ERB passing, s 1 500 300000 3754 286 16970 261774 1192 322 749 287904 8254 2 967 299193 8344 290 15300 267176 4827 323 695 287488 5364 3 1435 298387 10430 291 14432 267982 324 610 287072 4887 4 1903 297580 11324 292 14094 268789 5483 325 545 286656 5 2371 296774 12158 293 13556 269595 326 978 286239 6 2839 295967 294 13453 270402 6198 327 1443 285823 7 3306 295161 12098 295 12234 271208 6556 328 1923 285407 8 3774 294354 13410 296 12197 272015 7152 329 2389 284990 9 4241 293548 13112 297 11745 272821 6377 340 2821 284574 10 4709 292741 11979 298 11267 273627 341 3345 284158 11 5177 291935 299 10765 274434 342 3756 283742 12 5645 291129 300 10362 275240 343 4223 283325 13 6112 290322 14006 301 9852 276047 344 4746 282909 14 6580 289516 13529 302 9387 276853 6079 345 5114 282493 15 7048 288709 12277 303 8923 277660 9536 346 5656 282076 16 7516 287903 5721 304 8454 278466 12814 347 6187 281660 17 7983 287096 7569 305 7985 279273 348 281244 18 8451 286290 306 7513 280079 349 7067 280828 19 8919 285483 307 7025 280886 350 7523 280411 20 284677 308 6576 281692 351 7945 279995 21 9854 283870 309 6108 282498 352 8464 279579 22 10322 283064 310 5634 283305 353 8912 279162 23 10790 282258 311 5176 284111 354 9345 278746 24 11258 281451 312 4512 284918 355 9867 278330 25 11725 280645 313 3041 285724 356 10358 277914 26 12193 279838 314 2130 286531 357 10690 277497 27 12661 279032 315 1423 287337 358 11298 277081 28 13129 278225 316 912 288144 359 11754 276665 29 13596 277419 317 767 288950 360 12243 30 14064 276612 318 519 289757 361 12591 275832 31 14532 275806 319 623 289153 362 13049 275416 32 15000 275000 320 689 288737 363 13516 275012 36 16870 271774 321 754 288321 The time intervals of the satellite passing of the ERB

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

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

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

The time variation of protons flux (sm-2 s-1 sr-1) at 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

The time variation of protons flux (sm-2 s-1 sr-1) at 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

The time variation of protons flux (sm-2 s-1 sr-1) 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

The time and altitude variation of 4He flux (sm-2 s-1 sr-1) 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

The time and altitude variation of 12C and 16О flux (sm-2 s-1 sr-1) flux, cm-2s-1sr--1 С > 512 MeV С > 100 MeV 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 > 100 MeV The time and altitude variation of 12C and 16О 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

The preliminary estimations of averaged fluxes of GCR protons and helium nuclei Energy, MeV flux, 2,710-1 protons nuclei 4He 12C 16O >100 2,710-1 2,610-2 7,210-4 6,710-4 >512 2,310-1 1,910-2 5,410-4 5,110-4 >103 1,810-1 1,410-2 3,910-4 3,710-4 >104 9,210-3 5,310-4 1,510-5 1,610-5

Accumulated in Si for 7 years total doses dependence on spherical aluminium shield thickness

THEMIS, 2011

Ulysis

GEOTAIL, 1994 #302 #225

The estimations of averaged background fluxes of protons and electrons in the experiments GEOTAIL and Ulysis, cm-2s-1sr-1 Energy, MeV >0,038 >0,11 >0,34 1-3 5-10 protons 0,7 0,3 electrons 10 0,04* 0,003* *Now these data presented without efficiency of registration

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-1 for 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10-1 cm-2s-1sr-1 for protons with energy E>100 MeV in the telescope working area

Thank you for attention !!!!

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

Ulysis