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L. G. Sveshnikova1 , O. N. Strelnikova, L. A. Kuzmichev, V.S. Ptuskin, V.A. Prosin, E.Korosteleva et al

Nearby sources in the transition region between Galactic and Metagalactic cosmic rays

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L. G. Sveshnikova1 , O. N. Strelnikova, L. A. Kuzmichev, V.S. Ptuskin, V.A. Prosin, E.Korosteleva et al. Nearby sources in the transition region between Galactic and Metagalactic cosmic rays. - PowerPoint PPT Presentation

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Page 1: Nearby sources in the transition region between Galactic and Metagalactic cosmic rays

L. G. Sveshnikova1 , O. N. Strelnikova, L. A. Kuzmichev, V.S. Ptuskin, V.A. Prosin,

E.Korosteleva et al

Page 2: Nearby sources in the transition region between Galactic and Metagalactic cosmic rays

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

105 106 107 108 109 1010 1011

106

107

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.

Page 3: Nearby sources in the transition region between Galactic and Metagalactic cosmic rays

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

Page 4: Nearby sources in the transition region between Galactic and Metagalactic cosmic rays

Nearby sources from gamma-catalogs

3 kpc

Page 5: Nearby sources in the transition region between Galactic and Metagalactic cosmic rays

103 104 105 106 107 108 109 1010102

103

104

105

106

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

Page 6: Nearby sources in the transition region between Galactic and Metagalactic cosmic rays

105 106 107 108 109 1010 1011105

106

107

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

105 106 107 108 109 1010 1011105

106

107

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

Page 7: Nearby sources in the transition region between Galactic and Metagalactic cosmic rays

If we subtract the contribution of knee, how much is left over?

107 108 109 1010 1011105

106

107

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

107 108 109 1010 1011105

106

107

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

Page 8: Nearby sources in the transition region between Galactic and Metagalactic cosmic rays

First interpretation : Galactic sources : Expected source spectrum .

107 108 109 1010 1011105

106

107

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

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

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

Page 9: Nearby sources in the transition region between Galactic and Metagalactic cosmic rays

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

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

103 104 105 106 107 108103

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

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

Page 10: Nearby sources in the transition region between Galactic and Metagalactic cosmic rays

How many sources we expectand where should be the closest one?It depends on birthrate

0 2000 4000 6000 8000 100000

50

100

150

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

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

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

Page 11: Nearby sources in the transition region between Galactic and Metagalactic cosmic rays

Contribution of real nearby sources if they emits the same number of cosmic rays as an average SNR.

106 107 108 109 1010 1011 1012103

104

105

106

107

108

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,

Page 12: Nearby sources in the transition region between Galactic and Metagalactic cosmic rays

Cas A – very good candidate

107 108 109 1010105

106

107

3

.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

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

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.

Page 13: Nearby sources in the transition region between Galactic and Metagalactic cosmic rays

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

Page 14: Nearby sources in the transition region between Galactic and Metagalactic cosmic rays

Alternative explanation (If Metagalactic CR)

107 108 109 1010 1011105

106

107

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

107 108 109 1010 1011105

106

107

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

107 108 109 1010 1011105

106

107

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

“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

Page 15: Nearby sources in the transition region between Galactic and Metagalactic cosmic rays

It is easy to obtain some bumpor peak at the boundary between Galactic and Metagalactic CR

107 108 109 1010 1011105

106

107

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

Galactic CR- Meta Galactic CRsignature

Page 16: Nearby sources in the transition region between Galactic and Metagalactic cosmic rays

Main signatures: FePr at 2 10^17 эВVery low anisotropy at E>2 10^ 17

Page 17: Nearby sources in the transition region between Galactic and Metagalactic cosmic rays

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???

Page 18: Nearby sources in the transition region between Galactic and Metagalactic cosmic rays

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.

 

   

Page 19: Nearby sources in the transition region between Galactic and Metagalactic cosmic rays

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.

Page 20: Nearby sources in the transition region between Galactic and Metagalactic cosmic rays
Page 21: Nearby sources in the transition region between Galactic and Metagalactic cosmic rays

Contribution of nearby sourcesaround the knee

103 104 105 106 107 108 109 1010102

103

104

105

106

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

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

103 104 105 106 107 108 109 1010102

103

104

105

106

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

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

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!!!

Page 22: Nearby sources in the transition region between Galactic and Metagalactic cosmic rays

“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.

Page 23: Nearby sources in the transition region between Galactic and Metagalactic cosmic rays

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

Page 24: Nearby sources in the transition region between Galactic and Metagalactic cosmic rays