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What do we know about the
identity of CR sources?
Boaz Katz, Kfir BlumEli Waxman
Weizmann Institute, ISRAEL
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The cosmic-ray spectrum & Composition
Cosmic-ray E [GeV]
log [dJ/dE]
1 106 1010
E-2.7
E-3
Heavy Nuclei
Protons
Light Nuclei?
Galactic
X-Galactic)?(
[Blandford & Eichler, Phys. Rep. 87; Axford, ApJS 94; Nagano & Watson, Rev. Mod. Phys. 00]
Source: Supernovae)?(
Source?
Source?Lighter
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Intra-cluster CRs
• Observed in radio, HXR• Will not be discussed here
• See D. Kushnir’s talk: [arXiv:0903.2271, 0903.2275, 0905.1950]
* Likely origin- Accretion shocks * Predictions for Fermi, TeV (HESS, MAGIC)
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Galactic CR sources: Constraints
• Max >~1015eV
• Energy production rate LG,CR~(AdiskhCR)UCR/tCR
* UCR~1 eV/cm3,
* Propagation: 2nd-ary (& primary) composition
LG,CR~cAdiskUCR(disk/sec)~1049.5erg/100yr
25.0
secsec g/cmGeV10
/7.8,)/()(
Z
Zm
n
mnnij p
ii
p
ijji
[Blandford & Eichler, Phys. Rep. 87; Axford, ApJS 94]
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Galactic CR sources: SNe?
• Motivation for SNe as sources: * LG,CR~10-1.5 LG,SN
* Max ~1015eV * e- acceleration to 1015eV from X emission
• TeV photons from SNRs (RXJ1713.7-3946,RXJ0852.0-4622)
* Claim: must be due to pp pion production Confirms CR ion production
[e.g. Koyama et al. 95]
[e.g. Aharonian et al. 04--07]
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TeV must be due to e- IC
• pp origin in contradiction with radio, thermal-X
(non detection of thermal X n<~0.1/cm3):
• TeV consistent with e- IC, including “cutoffs”:
• Claims RE e- IC inconsistency: Detailed spectral shape near hc, where
theoretical predictions are highly uncertain
100
10
/
cm/1.05
1GHz
TeV
1
23.
L
Ln
L
L pe
Synch
pp
2
..
10BermTherm
pp
L
L
TeVcm/1.0
10,keVcm/1.0
11
3,
1
3.,
nh
nh cICcSynch
[Katz & Waxman 07]
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SNR TeV lessons
• Search at high n SNRs: Strong Thermal X, weak non-Thermal
• Difficult to prove pp based on EM obs. Highly simplified, phenomenological models (and plenty of room for complications: inhomogeneous plasma, particle spectra…)
[Katz & Waxman 07]
3
1
2
GeV1cm/110
/3
n
L
L pe
IC
pp
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PAMELA: New e+ sources?
• Apply
anti-p, e+ consistent with 2ndary origin
• Radiative e+ losses- depend on propagation in Galaxy (poorly understood)
* At 20GeV: frad~0.3~f10Be
* Above 20GeV: If PAMELA correct slightly rising frad()[Katz, Blum & Waxman 09]
)/()( sec Zm
n
mnnij p
ii
p
ijji
pp /
)/( eee
410
310
210
110
GeV10 GeV100
radf
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What do we know about >1019eV CRs?
• Max : LB>1012 (2/) (/Z 1020eV)2 Lsun
(see Dermer’s talk)
• Composition
[Waxman 95, 04]
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Composition clues
HiRes 2005
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Westerhoff (Auger) 2009
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What do we know about >1019eV CRs?
• Max : LB>1012 (2/) (/Z 1020eV)2 Lsun
• Composition: HiRes –protons, Auger- becoming heavier @
3x1019eV? !!Uncertain interaction cross sections
• Energy production rate: - LB>1012 Lsun & RL=/eB=40p,20kpc Likely X-
Galactic
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[Waxman 1995; Bahcall & Waxman 03]
[Katz & Waxman 09]
• 2(dN/d)=2(dQ/d) teff. (teff. : p + CMB N +
Assume: p, dQ/d~(1+z)m-
• >1019.3eV: consistent with protons, 2(dQ/d) ~1043.7 erg/Mpc3 yr + GZK
• 2(dQ/d) ~Const.: Consistent with shock acceleration [Reviews: Blandford & Eichler 87; Waxman 06
cf. Lemoine & Revenu 06]
Flux & Spectrum
cteff [Mpc]GZK (CMB) suppression
log(2dQ/d) [erg/Mpc2 yr]
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G-XG Transition at 1018eV?
Fine tuning Inconsistent spectrum
[Katz & Waxman 09]
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What do we know about >1019eV CRs?
• Max : LB>1012 (2/) (/Z 1020eV)2 Lsun
• Composition HiRes –protons, Auger- becoming heavier Uncertain interaction cross sections
• Energy production rate - LB>1012 Lsun & RL=/eB=40p,20kpc Likely X-
Galactic - Consistent with protons, 2(dQ/d) ~1043.7 erg/Mpc3 yr + GZK
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UHE CR sources• Constraints: - L>1012 (2/) Lsun
- 2(dQ/d) ~1043.7 erg/Mpc3 yr
- d(1020eV)<dGZK~100Mpc
!! No L>1012 Lsun at d<dGZK Transient Sources
• Gamma-ray Bursts (GRBs) ~ 102.5, L~ 1019LSun L/2 >1012 Lsun
(dn/dVdt)*E~10-9.5 /Mpc3 yr *1053.5erg ~1044 erg/Mpc3 yr Transient: T~10s << Tp~105 yr
• Active Galactic Nuclei (AGN, Steady): ~ 101 L>1014 LSun= few brightest
!! Non at d<dGZK Invoke:
* “Dark” (proton only) AGN * L~ 1014 LSun , t~1month flares
(from stellar disruptions)
[Blandford 76; Lovelace 76]
[Waxman 95, Vietri 95, Milgrom & Usov 95]
[Waxman 95]
[Boldt & Loewenstein 00]
[Farrar & Gruzinov 08]
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Anisotropy
• Cross-correlation signal: Inconsistent with isotropy @ 98% CL (~1.5) Consistent with LSS
• If anisotropy signal real & no anisotropy at 60EeV/(Z~10)
primaries must be protons See M. Lemoine’s talk [arXiv:0907.1354]
Biased (source~gal for gal>gal )
[Kashti & Waxman 08]
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The GRB “GZK sphere”
• LSS filaments: D~1Mpc, fV~0.1, n~10-6cm-3, T~0.1keV
B=(B2/8nT~0.01 (B~0.01G), B~10kpc
• Prediction:
p
D
B
few~)eV103( 20GRBsN[Waxman 95; Miralda-Escude &
Waxman 96, Waxman 04]
BBVGRBs
GRB
BBVp
DelaySpread
BBVp
fDN
R
fDd
c
d
fDd
2220
3
2
2
2052
2/1
20
2/10
10~)eV10(
yrGpc/5.0~
eV10/
Mpc100/yr10~~~
eV10/
Mpc100/3.0
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Summary• Galactic <1015eV (<1019eV) - LG,CR~10-1.5 LG,SN & Max ~1015eV (1019eV)
suggest SNR (trans-rel. SN) sources - TeV from low n, non-thermal X SNR: e- IC - Search for pp in high n, strong thermal X SNR pp:IC[@1GeV]~3 (n/1cm3) * Anti-p, e+ data consistent with 2ndary origin Prediction: e+/(e++ e-)<0.2+-0.1 up to ~300GeV PAMELA slightly rising frad() [constrain CR prop. Models]
• X-Galactic >1019eV - Likely protons, 2(dQ/d) ~1043.7 erg/Mpc3 yr, LB>1012 Lsun
suggest: GRBs [AGN flares?] - Anisotropy constrains primary composition
• Difficult to uniquely identify sources via EM observations Search for HE ’s
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Back up slides
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X-ray filaments
• Claim: X-ray filaments require B>100G, much larger than required for IC explanation of TeV emission (B~10G).
• Claim based on the assumption: Filaments due to e- cooling (vs, e.g., B
variations). * No independent support to this assumption; * X-ray & RADIO filaments (Tycho, SN2006)
inconsistent with this assumption.
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What is the e+ excess claim based on?
• On assumptions not supported by data/theory* primary e- & p produced with the same
spectrum, and e- and e+ suffer same frad
e+/e-~sec~-0.5
Or* detailed assumptions RE CR propagation, e.g. isotropic diffusion, D~, within an -independent box frad ~(-1)/2
• If PAMELA correct, these assumptions are wrong
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(Correct) detailed CR propagation models must agree with simple, analytic results
derived from sec
• Example: Diffusion models with {D~K0 , box height L}
reproduce data for parameter combinations shown in fig. [Maurin et al. 01]
• Trivial explanation: [Katz, Blum & Waxman 09]
Require sec( =35GeV) to agree with the value inferred from B/Csec =[3.2,3.45,3.9] g/cm2
[green, blue, red]
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The 1020eV challenge
RB eBRBR
R
BR
ccV p c
v
c
v
v/
1~
1 2
cec
BRL p
222
v/2
1v
84
v
v
sun122
20,
2
46
2
20
2
L10
erg/s10eV10/v
p
p
cL
2R
tRF=R/c)
l =R/
2 2
[Waxman 95, 04, Norman et al. 95]
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Anisotropy clues: I
Galaxy density integrated to 75MpcCR intensity map (source~gal)
[Waxman, Fisher & Piran 1997]
• Auger collaboration: Correlation with low-luminosity AGN @ 99% AGN? • AGN trace LSS Correlation with large-scale structure? Unfortunately… Unclear.
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GRB proton/electron acceleration
Electrons• MeV ’s:
• <1:
• e- () spectrum:
• e- ()energy production
erg/s1051L
5.210
2/ eee ddn
yrMpc
erg10erg10
yrGpc
10~
34452
32
e
ee d
nd
yrMpc
erg10erg10
yrGpc
5.03
445.533
[Waxman 95, 04] Afterglow, RGRB~SFR
Protons• Acceleration/expansion:
• Synchrotron losses:
• Proton spectrum:
• p energy production:
erg/s10/1025.22
20,5.50 pL
4/14/320,
2 ms10/10 tp
2/ ppp ddn
yrMpc
erg10
34422
e
ee
p
pp d
nd
d
nd
52
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GRB Model Predictions
[Miralda-Escude & Waxman 96]