L. G. Sveshnikova1, O. N. Strelnikova, L. A. Kuzmichev, V.S. Ptuskin, V.A. Prosin, E.Korosteleva et al.
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L. G. Sveshnikova1 , O. N. Strelnikova, L. A. Kuzmichev, V.S. Ptuskin, V.A. Prosin,
E.Korosteleva et al
Amazing fine structure in the range 10^16-10^18eV and highcontent of Fe around 10^17 eV eV in Tunka 133 and Kascade Grande
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Tunka133 Fe_Tunka Tunka25 Kascade Gr. Fe Kasc. Gr. Kascade EASTOP Tibet Augergv Hires1M3 Hires1 Hires2
F(E
) E
3.0
E, GeV
Tunka133-Heavy
Kask-Grandeheavy
Is it possible to indicate the sources giving the main contribution around the transition region 10^17-
510^18 eV?What can we say about source spectrum and
birthrate and candidates.
Sveshnikova L. G., Strelnikova O. N., Ptuskin V. S. On probable contribution of nearby sources to anisotropy and spectrum of cosmic rays at TeV-PeV-energies, Proc of 32 ICRC, Beijing, China, 2011, N 1057, 4p.
Basic MODEL of composition and Emax of Galactic sources at high energies:
sources are spread continuously in space and time
SSЫ
Type IIP SNRs (Emax~0.1Z PeV) <100 TeV
Type Ia SNRs (Emax~4Z PeV).
Type Ib/c SNRs (Emax~1Z PeV)
Type IIb SNRs (Emax~600Z PeV) 3-5%
V. Ptuskin, V. Zirakashvili, and Eun-Suk Seo, Spectrum of galactic cosmic rays accelerated in supernova remnants. Astrophysical J. T. 718 p. 31–36. 2010 Pmax/Z ∼ 1 × 1015×E51×n1/6M−2/3
ej
Nearby sources from gamma-catalogs
3 kpc
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ATIC-2; Tibet QGSJet Tunka-133; Kascade-Grande Calculation
F(E
)*E
2.7
m-2 s
-1 s
r-1 G
eV
1.7
E (GeV)
CC_SNR
SN IIb
SN Ia
d e m o d e m o d e m o d e m o d e m o
d e m o d e m o d e m o d e m o d e m o
d e m o d e m o d e m o d e m o d e m o
d e m o d e m o d e m o d e m o d e m o
d e m o d e m o d e m o d e m o d e m o
d e m o d e m o d e m o d e m o d e m o
Zirakashvili, V.N and Ptuskin, V.S.), Proc of 32 ICRC, Beijing, 2011,Zirakashvili, V.N., Aharonian, F.A., 2010, arXive: 1011.4775
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Si
CNOHe
P
ZZ14
Z
Z
Tunka133 Tunka25 Kascade Gr. Kascade EASTOP Tibet Augergv Hires1M3 Hires2
Fe_Tunka Fe Kasc. Gr.
F(E
) E3
.0
E, GeV
Z1
All
d e m o d e m o d e m o d e m o d e m o
d e m o d e m o d e m o d e m o d e m o
d e m o d e m o d e m o d e m o d e m o
d e m o d e m o d e m o d e m o d e m o
d e m o d e m o d e m o d e m o d e m o
d e m o d e m o d e m o d e m o d e m o
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Si
CNOHe
P
ZZ14
Z
Z
Tunka133 Tunka25 Kascade Gr. Kascade EASTOP Tibet Augergv Hires1M3 Hires2
Fe_Tunka Fe Kasc. Gr.
F(E
) E3
.0
E, GeV
Z1
All
width~26
We can directly obtain the chemical composition around the knee if we suppose the 1)regidity dependent Emax~ZEmax(pr),2)nearly same slopes for species, then we drow parallel lines
Nearly “normal” composition P+He(~70%) CNO(10%) Si-Ca(~10%),Fe (~15-25%) –small excess of Fe
If we subtract the contribution of knee, how much is left over?
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Galactic Tunka 133 Full KasC-Gran. Hires1 AugerLow Augergv
Meta From Tunka KGRaz
3
.0
FxE
E (GeV)
d e m o d e m o d e m o d e m o d e m o
d e m o d e m o d e m o d e m o d e m o
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d e m o d e m o d e m o d e m o d e m o
d e m o d e m o d e m o d e m o d e m o
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Galactic Tunka 133 Full KasC-Gran. Hires1 AugerLow Augergv
Meta From Tunka KGRaz
3
.0
FxE
E (GeV)
d e m o d e m o d e m o d e m o d e m o
d e m o d e m o d e m o d e m o d e m o
d e m o d e m o d e m o d e m o d e m o
d e m o d e m o d e m o d e m o d e m o
d e m o d e m o d e m o d e m o d e m o
d e m o d e m o d e m o d e m o d e m o
First interpretation : Galactic sources : Expected source spectrum .
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Galactic Tunka 133 Full KasC-Gran. Hires1 AugerLow Augergv
Meta From Tunka KGRaz
3
.0
FxE
E (GeV)
= -1.7+_0.2=-3.4
d=~1.7-1.9
Emax(Pr)=(2-3)10^17eVEmax(Fe)=(5-8)E^18
Width ~26
d e m o d e m o d e m o d e m o d e m o
d e m o d e m o d e m o d e m o d e m o
d e m o d e m o d e m o d e m o d e m o
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d e m o d e m o d e m o d e m o d e m o
1) The sharp knee with slope g ~1.7+-0.2 and
dg~2 (not 0.5) 2) Large dg means
light composition: P (70%),He(25%),
+CNO(1.5%),Si-Ca (1.5%), Fe (1%)
3) We expect significant contribution from one sources, because we could not imagine the class of sources with fixed Emax, due to large diversity of SNR properties
There is an optimal distance and time to reach the Earth for CR ~ 10^17 eV
103 104 105 1061E-4
1E-3
0,01
0,1
1
RSNR
=1 kpc
F E
3
T (years)
Energy 100 GeV 1 TeV 10 TeV 100 TeV 1 PeV
1 PeV
1 TeV
d e m o d e m o d e m o d e m o d e m o
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104
105
10^17 eV
Time of light propagation
TIm
e of
Cos
mic
Ray
Pro
paga
tion
Energy , GEV
Time
Time of CR propagation from 1 kpc D~ E^ 1/3
d e m o d e m o d e m o d e m o d e m o
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How many sources we expectand where should be the closest one?It depends on birthrate
0 2000 4000 6000 8000 100000
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at Rate=1/5000 yr (1% from all SNR) closest young sourcemost probably is located at ~3 kpc
Rel
ativ
e c
ount
s
Rmin (parsec)
d e m o d e m o d e m o d e m o d e m o
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If birthrate of sources (accelerated to 2E17)
1-3% from all, then the total number~1-3 sources within the
distance 3 kpc from Earth and younger 100 ky
The closest sources most probably is located
at 2-4 kpc
Contribution of real nearby sources if they emits the same number of cosmic rays as an average SNR.
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Kepler CasA) Tycho Crab RCW86 1006
3
.0
FxE
E (GeV)
J1713 Tcor
SN 1006, if r=4.4 kpc
g=2.1
Young Galactic SNRs (R~ 2-3 kpc, T~0.5-1.5
ky) – the best candidates,
Everyone from them can provides the CR in the region 10^17-5 10^18
эВ.
One evident problem!!!
We should see this source in gamma rays with very large
shock velocity, with very large turbulent magnetic field at the
shock front , small ejected mass,
Cas A – very good candidate
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.0
FxE
E (GeV)
CAS A (SNR of IIb type - nearest )
Source spectrum -2.02Emax=210^17 eVtwice power for CR prod. Light compositionFe~2%
d e m o d e m o d e m o d e m o d e m o
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Many unusual properties from (J. Vink. arXiv:1112.0576v2 ) J 1. An important class of SNRs are the so-called oxygen-rich SNRs. Chevalier and Oishi (2003) : Cas A must have been a Type IIb SNR, similar to SN1993J 2.Progenitor main sequence mass of 18±2M .⊙4. Strong bipolarity referred to as “the jet”. 5. Best explained with a binary star scenario, in which a high mass loss is caused by a common envelope phase. 6. In Cas A many iron-rich knots, indicate that the mean velocity of these iron knots are higher than 7000 kms−1.
Main Signatures of this hypothesis:
Chemical composition around 1018 should be lnA ~2 - not lighter
Very high anisotropy at 2 10^17-5 10^18
Alternative explanation (If Metagalactic CR)
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Galactic Tunka 133 Full KasC-Gran. Hires1 AugerLow Augergv
Meta From Tunka KGRaz
3
.0
FxE
E (GeV)
d e m o d e m o d e m o d e m o d e m o
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d e m o d e m o d e m o d e m o d e m o
d e m o d e m o d e m o d e m o d e m o
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Galactic Tunka 133 Full KasC-Gran. Hires1 AugerLow Augergv
Meta From Tunka KGRaz
3
.0
FxE
E (GeV)
d e m o d e m o d e m o d e m o d e m o
d e m o d e m o d e m o d e m o d e m o
d e m o d e m o d e m o d e m o d e m o
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d e m o d e m o d e m o d e m o d e m o
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Galactic Tunka 133 Full KasC-Gran. Hires1 AugerLow Augergv
Meta From Tunka KGRaz
3
.0
FxE
E (GeV)
d e m o d e m o d e m o d e m o d e m o
d e m o d e m o d e m o d e m o d e m o
d e m o d e m o d e m o d e m o d e m o
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d e m o d e m o d e m o d e m o d e m o
d e m o d e m o d e m o d e m o d e m o
“Inhomogeneous extragalactic magnetic fields and the second knee in the cosmic ray spectrum”. K. Kotera and M. Lemoine arXiv:0706.1891v2 [astro-ph] 4 Jan 2008Variant :Bo=2 nG, lc=100 kpc, n=1-^-5 Mpc-3
It is easy to obtain some bumpor peak at the boundary between Galactic and Metagalactic CR
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.0
FxE
E (GeV)
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Galactic CR- Meta Galactic CRsignature
Main signatures: FePr at 2 10^17 эВVery low anisotropy at E>2 10^ 17
I )Conclusion: if Galactic sources provide CR between CR in 10^17-410^18: 1) Sources spectrum: ~ 1.7-2.01, Emax ~ z(23)1017 , very light composition
P+He~95%, Fe<2%
2) Closest sources should be at distance ~2-4 kpc, T < 100 ky
3) One source with usual power is enough, may be Cas A???
II.Conclusion GalacticMetagalactic at 10^17 eV
The variant Galactic Metagalactic CR at 10^17 eV does not contradict to calculations with magnetic horizon
and to chemical composition measured in Hires and Telescope array,
and even it is possible to get a bump or peak at the boundary.
Conclusions 3
The fine structure and the high content of Fe around 1017 eV can be reproduced in the model if class of sources SNIa (standard candles in cosmology, birthrate ~20% from all) with Emax ~4 PeV and chemical composition P+He~ 60%, Fe~15-25~%, d~2 in source.
Contribution of nearby sourcesaround the knee
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Vela Jr (0.3 kpc 0.7 ky)
ATIC-2; Tibet QGSJet Tunka-133; Kascade-Grande Calculation
F(E
)*E
2.7
m-2 s
-1 s
r-1 G
eV
1.7
E (GeV)
HB9
Cygnus Loop
HB21
Vela Jr. (0.7 kpc 1.7 ky)
d e m o d e m o d e m o d e m o d e m o
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Vela Jr (0.3 kpc 0.7 ky)Emax=F(Temissin)
ATIC-2; Tibet QGSJet Tunka-133; Kascade-Grande Calculation
F(E
)*E
2.7
m-2 s
-1 s
r-1 G
eV
1.7
E (GeV)
HB9
Cygnus Loop
HB21
Vela Jr. (0.7 kpc 1.7 ky)
d e m o d e m o d e m o d e m o d e m o
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We could not exclude the “single source”
But only Vela Jr. can provide the structure around the knee and
only if :1)Emax=F(Temission
)2)D~0.3 kpc, T~0.7
ky
It’s very difficult to obtained high Fe content
around 10^17 eV.Background sources also
must have high Fe content!!!
“Single source “
III. Only one sources -Vela Jr – if it is very young and close if (R~0.3-0.5 kpc, T~0.7-1.7 ky,) is suited to the “single source” determining the “sharpness” of the knee,
But the background also should be
abundant with by Fe nuclei in the region 10^17 ev, that in their turn means the rigidity dependent knee around 4 PeV for background sources also.
Zirakashvili, V.N and Ptuskin, V.S.), Proc of 32 ICRC, Beijing, 2011, Role of reverse shocks for the production of galactic cosmic rays in SNRs Zirakashvili, V.N., Aharonian, F.A., 2010, arXive: 1011.4775
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