Radiation conditions during the GAMMA-400 observations:

orbit, doses and particles fluxes

GAMMA-400 at the NAVIGATOR-2` satellite platform

0 2 4 6 8

0

100000

200000

300000

Hкм .

Hкм .

H

H

t, год

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 MeVThe 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 raysSolar 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 < 30MeV)).

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

The integral electrons count rate maps in the band Е>1 MeV (AE-8 MAX model)

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 backgroundlow altitude orbit

data

residial

model

residial

0 1000 2000 3000 400030000 31000 320000.01

0.1

1

10

100

1000

10000

100000

tbad1

~220000s=8,5%

tbad2

~280000s=11%

ttot

~2600000s

time, s

flu

x,

arb

. u

nit

s

1000 10000 10000010-4

10-3

10-2

10-1

100

101

102

103

104

flu

x,

arb

. u

nit

s

time, s

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

t, days

№ orbit perigee,km

apogee, km

Вtime of ERB passing, s

№ orbit

perigee,km

apogee, km

Вtime of ERB passing, s

№ orbit perigee,km

apogee, km Вtime of ERB passing, s

1 500 300000 3754 286 16970 261774 1192 322 749 287904 82542 967 299193 8344 290 15300 267176 4827 323 695 287488 53643 1435 298387 10430 291 14432 267982 5364 324 610 287072 48874 1903 297580 11324 292 14094 268789 5483 325 545 286656 37545 2371 296774 12158 293 13556 269595 4887 326 978 286239 83446 2839 295967 10430 294 13453 270402 6198 327 1443 285823 104307 3306 295161 12098 295 12234 271208 6556 328 1923 285407 113248 3774 294354 13410 296 12197 272015 7152 329 2389 284990 121589 4241 293548 13112 297 11745 272821 6377 340 2821 284574 1043010 4709 292741 11979 298 11267 273627 6556 341 3345 284158 1209811 5177 291935 8344 299 10765 274434 6556 342 3756 283742 1341012 5645 291129 12098 300 10362 275240 7152 343 4223 283325 1311213 6112 290322 14006 301 9852 276047 6556 344 4746 282909 1197914 6580 289516 13529 302 9387 276853 6079 345 5114 282493 834415 7048 288709 12277 303 8923 277660 9536 346 5656 282076 1209816 7516 287903 5721 304 8454 278466 12814 347 6187 281660 1400617 7983 287096 7569 305 7985 279273 7569 348 6556 281244 1352918 8451 286290 12814 306 7513 280079 5721 349 7067 280828 1227719 8919 285483 9536 307 7025 280886 12277 350 7523 280411 572120 9387 284677 6079 308 6576 281692 13529 351 7945 279995 756921 9854 283870 6556 309 6108 282498 14006 352 8464 279579 1281422 10322 283064 7152 310 5634 283305 12098 353 8912 279162 953623 10790 282258 6556 311 5176 284111 8344 354 9345 278746 607924 11258 281451 6556 312 4512 284918 11979 355 9867 278330 655625 11725 280645 6377 313 3041 285724 13112 356 10358 277914 715226 12193 279838 7152 314 2130 286531 13410 357 10690 277497 655627 12661 279032 6556 315 1423 287337 10430 358 11298 277081 655628 13129 278225 6198 316 912 288144 8344 359 11754 276665 637729 13596 277419 4887 317 767 288950 6556 360 12243 276665 715230 14064 276612 5483 318 519 289757 4827 361 12591 275832 655631 14532 275806 5364 319 623 289153 6556 362 13049 275416 619832 15000 275000 4827 320 689 288737 7152 363 13516 275012 488736 16870 271774 1192 321 754 288321 8344

Th

e ti

me

inte

rval

s o

f th

e sa

telli

te p

assi

ng

of

the

ER

B

0 10 20 30 40 50

0,0

100

101

102

103

104

105

106

107

108

по

то

к, с

м-2

с-1

L

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

flu

x, c

m-2

s-1

1 10 100 1000 10000

0,01

0,1

1

пото

к, м

-2с-1

МэВ

-1ср

-1

Энергия, МэВ

C

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

energy, MeV

cm-2

s-1M

eV-1

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

energy, MeV

cm-2

s-1M

eV-1

100 1000 10000

0,01

0,1

1

10

время, с

по

то

к, с

м-2с

-1с

р-1

E > 300 МэВ

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)

590000 600000 610000

0,01

0,1

1

10

100

E > 300 МэВ

по

то

к, с

м-2с

-1с

р-1

время, с

1190000 1200000 1210000

0,01

0,1

1

10

100

E > 300 МэВ

время, с

по

то

к, с

м-2с

-1с

р-1

flu

x, c

m-2s-1

sr--

1

flu

x, c

m-2s-1

sr--

1

flu

x, c

m-2s-1

sr--

1

time, stime, s

time, s

100 1000 10000

0,01

0,1

время, с

по

то

к, с

м-2с

-1ср

-1

E > 500 МэВ

590000 600000 610000

0,01

0,1

E > 500 МэВ

по

то

к, с

м-2с

-1с

р-1

время, с

1190000 1200000 1210000

0,01

0,1

по

то

к, с

м-2с

-1с

р-1

время, с

E > 500 МэВ

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)

flu

x, c

m-2s-1

sr--

1

flu

x, c

m-2s-1

sr--

1

flu

x, c

m-2s-1

sr--

1

time, stime, s

time, s

100000 200000 300000 400000 500000

0,01

0,1

по

то

к, с

м-2с-1

ср

-1

время, с

E>1MeV E>10MeV E>50 MeV E>100MeV E>300MeV E>500MeV E>1GeV E>3GeV E>10 GeV

4,0x103 8,0x1035,94x105 5,945x105 5,95x105 5,955x105 5,96x105 5,965x105 5,97x105

0,01

0,1

время, с

по

то

к, с

м-2

с-1

ср-1

E>1MeV E>10MeV E>50 MeV E>100MeV E>300MeV E>500MeV E>1GeV E>3GeV E>10 GeV

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

flu

x, c

m-2s-1

sr--

1

flu

x, c

m-2s-1

sr--

1

time, s

time, s

100000 200000 300000 400000 500000

10-3

10-2

время, с

по

то

к, с

м-2с-1

ср-1

вы

со

та

, км

H2 He H3 H4 E3

5,0x104

1,0x105

1,5x105

2,0x105

2,5x105

3,0x105

6,050x103 5,940x105 5,945x105 5,950x105 5,955x105 5,960x105 5,965x105 5,970x10510-4

10-3

10-2

время, с

вы

со

та

, км

по

то

к, с

м-2с

-1ср

-1

H2 He H3 H4 E3

104

105

He >10 GeVHe >1 GeVHe >512 MeVHe >100 MeVр >10 GeV

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)

alti

tud

e, k

m

flu

x, c

m-2s-1

sr--

1

flu

x, c

m-2s-1

sr--

1

alti

tud

e, k

m

He >10 GeVHe >1 GeVHe >512 MeVHe >100 MeVр >10 GeV

time, s

time, s

100000 200000 300000 400000 5000001,4x10-5

1,45x10-51,5x10-5

1,55x10-51,6x10-5

1,65x10-51,7x10-5

4x10-4

5x10-4

6x10-4

7x10-4

8x10-4

пот

ок, с

м-2

с-1

ср-1

высо

та,

км

время, с

H10 H9

H11 H12 H13

H14 H15 H16

5,0x104

1,0x105

1,5x105

2,0x105

2,5x105

3,0x1056,050x103 5,940x105 5,945x105 5,950x105 5,955x105 5,960x105 5,965x105 5,970x105

1,4x10-51,45x10-51,5x10-5

1,55x10-51,6x10-51,65x10-51,7x10-5

3,5x10-4

4x10-4

4,5x10-4

5x10-45,5x10-4

6x10-46,5x10-4

7x10-47,5x10-4

8x10-4

пот

ок, с

м-2

с-1ср

-1

высо

та,

км

время, с

H10 H9

H11 H12 H13

H14 H15 H16

104

105

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 > 512 MeVС > 100 MeV

С > 1 GeVС > 10 GeVО > 100 MeV

О > 512 MeVО > 1 GeVО > 10 GeVfl

ux,

cm

-2s-1

sr--

1

flu

x, c

m-2s-1

sr--

1 С > 512 MeVС > 100 MeV

С > 1 GeVС > 10 GeVО > 100 MeV

О > 512 MeVО > 1 GeVО > 10 GeV

time, s

time, s

alti

tud

e, k

m

alti

tud

e, k

m

The preliminary estimations of averaged fluxes of GCR protons

and helium nuclei

Energy,MeV

flux, 2,710-1

protons

nuclei4He 12C 16O

>100 2,710-1 2,610-2 7,210-4 6,710-4

>512 2,310-1 1,910-2 5,410-4 5,110-4

>103 1,810-1 1,410-2 3,910-4 3,710-4

>104 9,210-3 5,310-4 1,510-5 1,610-5

0.1 1 1010-1

100

101

102

103

104

105

106

107

108

do

se

in

Si,

ra

d

shield thickness, mm

A=300000km,

Р=500km, i=51,8o, t=171.35h

total dose electrons

bremsstrahlungtrapped protons протоны

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

THEMIS, 2011

Ulysis

#225#302

GEOTAIL, 1994

Energy, MeV >0,038 >0,11 >0,34 1-3 5-10

protons 0,7 0,3 0,3

electrons 10 10 0,04* 0,003*

*Now these data presented without efficiency of registration

The estimations of averaged background fluxes of protons and electrons in the experiments

GEOTAIL and Ulysis, cm-2s-1sr-1

conclusionsVery 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 300000km) 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-2s-1 for protons with energy E>0.3 MeV inside the outer magnetosphere and 100 particles per cm-

2s-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 2,710-1 cm-2s-1sr-1 for protons with energy E>100 MeV in the telescope working area

Thank you for attention !!!!

1 10

0.01

0.1

1

10

100

1000

10000

100000

1000000

flu

x, c

m-2

s-1

sr-1

E>1 MeV E>10 GeV

L

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

100 1000 10000 100000 10000000.004

0.006

0.008

0.01

0.012

0.014

0.016

0.0180.02

time,s

flu

x, c

m-2s

-1s

r-1

E>10 GeV

Ulysis