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Дата изменения: Sun May 22 11:45:39 2011
Дата индексирования: Mon Feb 4 18:36:19 2013
Кодировка:

Fine structure, mass composition, peaks
..

GAMMA

STRUCTURE: -1 knees and pronounced peak,
5,0x10
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F(E)/AE-3

F(E)/AE

-2.9

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and TUNKA

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F(E)/Ae3-1

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Kascade Grande
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Kaskade Grande Eas Top

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-1,0
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EASS TP OP EA TO Tu ka TUNnKA
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Galstr Grandest B Tun133st C Tun25str B EasTpst Hires1st er2 KaskadeStr ### ### ###

F(E)/Ae3-1

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GAMMA
F(E)/AE
Galstr Tibetst EEr2 MGUstr Er3 ### ### ### ### ### ### ### ### ###

E, GeV
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-3.0

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Galstr Tibetst EEr2 MGUstr Er3 ### ### ### ### ### ### ### ### ###

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F(E)/Ae3-1

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Tibet (E-->E*1.26 in theory

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Tibet, MSU (E-->E*1.26 in theory

Tibet
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MSU
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EGv Line- our model one of calculate,deV ariants

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Basic MODEL:
V. Ptuskin, V. Zirakashvili, and Eun-Suk Seo, Spectrum of galactic cosmic rays accelerated in supernova remnants. Astrophysical J. T. 718 p. 3136.

Several types of SNR:
· 1. Type Ia SNRs (Emax~4Z PeV) with the following parameters: kinetic energy of explosion E = 1051erg, number density of the surrounding interstellar gas n = 0.1 cm-3, and mass of ejecta Mej = 1.4Ms can accelerate particles to the energy of the knee. 2. Type Ib/c SNRs (Emax~1Z PeV) with E = 1051 erg exploding into the low density bubble with density n = 0.01 cm-3 formed by a progenitor star as a WolfRayet star. The ejecta mass is Mej = 2Ms and k = 7. 3. Type IIP SNRs (Emax~0.1Z PeV) with parameters E=1051erg, n = 0.1 cm-3, Mej = 8M, and k = 12. 4. Type IIb SNRs (Emax~600Z PeV) with E = 31051 erg, n = 0.01cm-3, and Mej = 1Ms. Before entering the rarefied bubble, the blast wave goes through the dense wind emitted by the progenitor star during its final RSG stage of evolution. It was assumed that the mass loss rate by the wind is M = 10-4M yr-1 and the outer wind radius is 5 pc.

·

·

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In this model sources are distributed continiously, the random nature of sources Is not considered

Extension of this model takes into account a statistical nature of sources:
Nearby (Rnear~1.-1.5 ) and Young Tnear~105 ) are taken

from gamma astronomy catalogs

Distant and old sources are simulated randomly

The propagation time of 4 PeV protons is around 104 years (less than survival time of shells and PWNs, so we try to identify gamma-atronomy detected source and cosmic ray source.

Additional suggestings:
1) All SNR Ia (thermonuclear explosions accelerate up to Emax =4 PeV (23%)

2)

Collapsing SNR II, SNIbc have distributed Emax from 1 TeV to 1000 TeV:
This results in additional Earth
sour

d

~0.17, and observed near

obs=

+ d+ d

prop

~2.705

sour=2.2.

3) and 2-5 % SNIIn accelerated up to 6 1017 eV.
3) Chemical composition: 37% of H, 35% of He, 8% CNO, 10% of CNO, 8 % of intermediate nuclei, 10% of Fe.

Spectrum without propagation
· Structures can be explained only if the cutoff in source spectrum is strong d>2.5 -3.0 · Fe - peak can be explained only if we suggest "bump" before cutoff energy

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Protons

Sn_Ia (Emax=4 PeV)

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with bump before Emax

F(E) E

Main variant
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no peak

Sn_IIn(Emax=600 PeV)

F=E
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(1 +(E/Ek) )
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c/

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Total all particle spectrum in our model ( F(E)*E3) has fine structures
·

10 Galactic sources
E2knee=600 3.38E6

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1) bump around 4 PeV is produced by proton and helium nuclei with nearly equal abundances 2) concavity above 1016 eV denotes the transition to CNO and more heavier nuclei, the amount of Fe nuclei at that should be not less than 1/3 of He nuclei. 3) sharp break around the 108 GeV marks the transition to the contribution of rare SNIIb being able to accelerate protons up to 6x1017 eV comprising the several percents among all SNR. The slope of spectrum (-3.24+-0.08 in KG) in the model is connected with the slope of cutoff. 4) If we exclude SNIIb we can not describe the flat spectrum above the 1016 eV. 5) Two variant of calculation: Main 1 (absence of SNRs in the Earth vicinity with Emax=4 PeV) and Main 2 (where 4 SNRs accelerate to 4 PeV) give more or less similar structures around the knee

Here we need to know MetaGalactic
Sum Gal+Metag 025 0.20

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P

He

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Fe
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C,O Si

Pure Galactic ·

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Contribution of nearby actual sources
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Variant 1: No one SNR <1 kpc can accelerate to 4 PeV Total contruution: 7% in total

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Variant 2: all pure shell SNRs < 1 kpc accelerate to 4 PeV Total contribution 30% in total

We did not find the actual single sources that can imitate the fine structure

Variant without "bump" in source spectrum can not describe Fe-peak, but describe structures

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with peak no peak Sn_IIn(Emax=4x150 PeV)

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Variant with wide (0.5 order) "bump" in source spectrum can describe Fe-peak more or less

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with peak no peak Sn_IIn(Emax=4x150 PeV)

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Variant with narrow (0.25 order) "bump" in source spectrum can describe Fe-peak completely, but there is a some contradiction with the main knee it becomes too narrow and with 2 ears

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Sn_Ia (Emax=4 PeV)

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with peak no peak Sn_IIn(Emax=4x150 PeV)

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F=E
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(1 +(E/Ek) )
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Mass composition in 3-d variant coincides with Tunka -133 last data

Mass composition: 3 dif. variants
· 1) Emax (P) In Galaxy ; 4 PeV

· 2) Emax (P)=4 and 600 PeV This variant predicts a heavy composition at 1018 eV

·3) SNR Ia + He stars +MetaGalactic with mixed composition in sources

Implications of the cosmic ray spectrum for the mass composition at the highest energies D. Allard1, N. G. Busca1, G. Decerprit1, A. V. Olinto1;2, E. Parizot1

Figure 3. Propagated spectra obtained assuming a mixed source composition compared to HiRes (left) and Auger (right) spectra, the dierent components are displayed .

Variant with Meta-galactic with mixed composition and with
He-stars (without heavy nuclei) instead of SNIIn
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Galactica: SN Ia accelerate all nuclei to 4 PeV, SN IIn to 600 PeV, but only P, He (He stars).

He
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Fe

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P Metagalactika, mixed composition

Tun133 GrandeKas Hires1 Hires2 EASTOP Tibet KASKADE Tunka25 MGUIE3 AKENO Augergv Hires1M3

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Amplitude and Right ascension of anisotropy around the knee

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Compilation [9] Akeno, Yakutsk , KaskadeGrande KASCADE AUGER AGASA

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Vela Jun 0.3 kpc 700 y
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Right Ascension, hours

Anisotropy amplitude

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Calculation Vela Jun Main1 Main 2

Akeno []

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Energy, GeV

Conclusions about Fe-peak
· To get in our calculations Fe-peak we need to introduce some bump in source spectrum with a width 0.3 or 0.1 of the order. Single nearby source could not help in this problem. First a very impressive fact a very good coincidence of positions of the Fe peak and position of P-He main knee at the suggestion of normal composition. In the case of narrow peak (1/10 of order) Fe peak is reproduced perfectly , but the main knee should be visible as two knees. May be if we take into account an accuracy of energy and mass determination, it helps to smooth these peaks. The nature of the bump in a source spectrum is not clear fully. But it can reflect the time dependent emissions most energetic particles are emitted at the beginning of the acceleration process, when the speed of shock wave is maximal. This bump should be seen during 104 ears (time of collecting of PeV signal from the sources due to propagation) and should be variable in the time .

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Propagation Time for different energies
protons R=1 kpc
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100 GeV 1 TeV 10 TeV 100 TeV 1PeV

FE

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Age of SNR (years)

We can identified

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25 R <1.5 T <105 ( 73 3 ) SNR 6 ( , Ia (25%).

19 PWN (11 ) - (11 ), 19 HESS - 30 %,

6 SNR - 1 ( J1713-3946) .

HSWFP
_SW__ _SW__

L .
6 5 .3 6 5 .7

Dmn
0.8 1.5

T
20. 0.

Name
G65.3+5.7 DA495

_S___
_S_F_ _S___ _S__ _SWFP _S__P _SWF_ _S___ _S___ _SW_P _SW__ HSWFP HSWF_ HWFP HS___ H____ ___P _ _ _ FP __W__ _ _ _ FP __WF__ H _ _ F_

74.0
7 8 .2 8 9 .0 9 3 .7 1 0 6 .3 1 1 4 .3 1 1 9 .5 1 2 7 .1 1 6 0 .9 1 8 0 .0 1 8 9 .1 2 6 3 .9 2 6 6 .2 3 4 3 .1 3 4 7 .3 3 5 3 .6 4 9 .1 2 0 1 .1 2 9 1 .0 2 0 1 .2 7 .4 8 0 .2

0.44
1 .5 0 .8 1 .5 0 .8 0 .7 1 .4 1 .2 0 .8 0 .8 1 .5 0 .2 9 1 .3 1 .4 1 .0 0 .8 1 .4 0 .2 9 1 .0 0 .7 5 1 .7 1 .6

20.
7. 19. 120. 10. 7 .7 14. 0. 6 .6 4 .6 20. 1 1 .0 10. 18. 1 .6 27. 88. 110. 0. 44. 68. 120.

Cygn Loop
DR4 HB 21 CTB104,DA551 Boomerang G114.3+0.3 CTA R5 HB 9 S147 IC443, 3C157 Vela X Vela Jun. FermiG343.1 J1713-3946 HESSG353.6 PSRB1916 Monogem PWNG291.02-0.11 J0631+1036 J1809-2332 J2032+4127