18 may, 2006kaw4, daejeon1 astrophysical sources of uhecrs tom jones university of minnesota
TRANSCRIPT
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18 May, 2006 KAW4, Daejeon 1
Astrophysical Sources of UHECRs
Tom Jones
University of Minnesota
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Outline
•Observational constraints
•Basic physical limitations on sources
•Some astrophysical models
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All particle cosmic ray spectrum
UHECR
Nagano & Watson 00 LHC ppCM ZeV
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Spectrum below ~100EeV pretty well known
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Abbasi etal, ApJ 2005
Best Fit:80% p; QGSJet60% p; SIBYLL
UHECRComposition:could be almost all p
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eV
TeV
eV
xmmmE pep
18142210
~)(
105~
4
2
eV
T
xeV
eV
xmmmE pp
201622102
~)(
107~
4
cudtdEE
c
D
Propagation Issue 1:Protons > 0.1 ZeV severely limited by energy losseson CMB photons (Greisen-Zatsepin-Kuzmin; GZK)1,2
Photo-pairproduction
Photo-pionproduction
Path limit: is cross section is fractional energy loss
1 Assuming ‘standard physics’2 Also an accelerator issue using local photon field
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Resulting Propagation Limits Against CMB
Conditionsmatched tolook back time,adiabatic lossesincluded
ConcordanceCDM
Pair losses
Pion losses
‘GZK sphere’
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Abu-Zayyad etal, APh, 18, 237 (2002)
1 EeV 1 ZeV
Number of events:
EEeV > 10: ~ 103
EEeV > 40: ~ 100EEeV > 100: ~ 10
Do we see theGZK feature?HiRes vs AGASA
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Small statistics: photo-pion losses are discrete:GZK feature not yet confirmable
De Marco, Blasi & Olinto (APh, 20, 53 (2003))
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Propagation issue 2:What do arrival directions tell us About the sources?
>Nearly isotropic with perhaps some clustering and/or correlations with ‘interesting’ astrophysical objects
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Auger: Sky Map of Data set
Auger latitude= -36. Always sees South with limited coverage in North. Mantsch etal
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AGASA Small Scale Clustering for E >4x1019eV
• Isotropic in large scale Extra-Galactic• But, Clusters in small scale (Δθ<2.5deg)
– 1triplet and 6 doublets (2.0 doublets are expected from random)– One doublet triplet(>3.9x1019eV) and a new doublet(<2.6deg)
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Gorbunov etal 2004
BL Lac /UHECR Cross-correlations?
logE>19.5
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Deflection of Protons >41019eV(< 100 Mpc)
Dolag etal 2003
0o360o
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Astrophysical Source Energetics:Local energy density in 100 EeV CRsu~4J/c~3x10-22 J/m3~3x10-21 erg/cm3
loss~3x108yr, so
~u/loss~10-37 W/m3
~3x1044 erg/Mpc3/yr
Roughly equivalent to ~ 1 ‘AGN’ inside 100 Mpc (~2x10-7 Mpc-3)Or
Cosmic GRB rate ignoring evolution
Perhaps event cluster statistics gives a space density[Blasi & De Marco 2004] ~ 10-5 Mpc-3 from AGASA data
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Some Astrophysical Accelerator Issues
• How particles of such extreme energy (~1021 eV = 1 ZeV) can be accelerated and escape; i.e, what can make a “Zevatron”?
• How to match the GZK feature (flight < 108yr above ~100 EeV) if it exists or not (source spectrum)
• How to account for an essentially isotropic distribution of detections (sources & propagation), maybe with some correlations and clustering
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Emax: Some Standard Estimates for an Accelerator
•Containment: rg = (E)/(ZeB) < RE < ZeBR
•Unipolar inductor: E<ZeBR (R/c)~a ZeBR
•Diffusive shock acceleration (DSA) (nonrelativistic):acc ~ 10 /(u2
s) < R/us with rg cE < sZeBR
•Relativistic shock DSA (analogous argument):E < sZeBR
•All lead roughly to (Hillas):E < 0.9 Z BGauss Rpc ZeV
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“Hillas Plot” for some plausible accelerators (after Hillas 1984)
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Those estimates based on simple field models
Magnetic field amplification?For example, in shocks
(Bell & Lucek 2000)
Resonant wave instability:
202
20
2 ~~~
/~;~
Bv
PBMP
v
vBE
x
vxPvE
dx
dPv
dt
dE
s
cAc
s
Aw
d
sdcAw
cA
w
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Photo-pion production off Blackbody radiation
n =20 T3cm-3; E = 3.5x10-4T eV
Setting > R/c gives R < 1/(20T3)
Near threshold, E > 8x1019T-1 eV, cm-2; ~ 0.1
So propagation distance limited by
max(R, cacc) < 2.5x1026 cm (2.7/T)3 cm
Compact high luminosity accelerators probably eliminated:
*AGN (T~105K), R<0.3 AU for E>1014 eV *Near young neutron star (T ~ 3x107K), R<25 km for E>3x1012eV
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Some Models: Radio Galaxy Jet Terminal Shock (e.g., Rachen & Biermann 1993)
us > 0.1c; a>0.1R ~ 10 kpcB ~ 10-5-4 G
•Hillas constraint applied to DSA give E ~ 1 ZeV; acc > 105 yr
•Synchrotron & photo-pion losses give comparable limit
•Shear layer of relativistic jet (eg, Ostrowski 2002, Rieger & Duffy 2004)(similar to DSA, except boost E/E ~ j, so can be quickin principle. Escape still limits to Hillas constraint.
•RGs rare in the local universe, so isotropy from RGs inside GZK sphere requires nanoGauss intergalactic and/or 100 nanoGauss galactic halo magnetic fields to deflect arrival directions.
•Jet proton content uncertain
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BL Lac Jets
Possible correlation with BL Lacsrelativistic jets with ~ 10 beamed
our way
Local BLL density small, so same isotropy concerns already mentioned
If sources outside GZK sphere, then `X-bursts’,‘uhecrons’ ? (‘liberated’ superheavies, productsthat avoid or delay GZK)(Albuquerque etal 1998; Biermann & Frampton 2005)
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Cosmic structure shocksKang, Rachen & Biermann 1997
shocks thermal emission
Shock surfaces Thermal Emissivity
Cluster shocks are big (~ Mpc), moderately fast (~103km/sec),but B is weak (~< G), so E < few EeV by various arguments(e.g., Norman, Melrose & Achterberg 1995;Ostrowski & Siemieniec-Ozieblo 2002)
~20Mpcbox
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Larger shocks: sheets, filaments & ‘superclusters’
25h-1 Mpcbox
R ~ 10s of Mpcus ~ few 102
km/sec
B ~ 10-9-10-7 G?
E ~ 100 EeV ?
Not likely
Ryu, Kang, Hallman & Jones 2003
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Gamma Ray Bursts:e.g., Waxman 1995, 2000; Vietri 1995
Ultrarelativistic shocks in fireballs (jets):~1052-53 erg>300, with internal shocks from flow variations
Waxman 1995, 1999: DSA at internal shocks; R < 1016 cmIf B in equipartition with radiation, B~104 Gauss
E < ZeBR ~ 1020 eV(photopion losses not as restrictive,But synchrotron losses should limitE<1019 eV)Shock/Proton efficiency?Evolution constraints
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GRB Blast Wave Model
e.g., Vietri 1995; Gallant & Achterberg 1999; Vietri, De Marco & Guetta 2003
•If in ISM, insufficient time to reach UHE (G & A):E < 5x1015 BG (E52 3/n0)1/3 eV,= E /Mc2
•If in a Pulsar Wind Bubble, thenB ~ 0.1-10 G for R ~ 1016 cmE < 1020 3
2 iW eV,W is spin down luminosity,i is the proton mass fraction
•Energetics: If no evolution, then GRB ~ UHE
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Young Magnetar Winds
Arons (ApJ, 589, 871, 2003)
•Winds avoid large magnetospheric energy losses (Blasi, Epstein & Olinto 2000)~ 3x1022 33 (4)2 V available magnetic rotator voltage•Ion return current sheet may experience ~10% of •Wind can carry substantial fraction of spindown energy Spin down time ~ 5 I45/(33 4)2 minutes•Ions may ‘surf’ the wind•A fast magnetar birth rate ~ 10-5 /yr/galaxy & 10% efficiency for UHECR accounts for energetics•Injection spectrum ~ E-1 steepening to E-2 if early GR spindown•Is the wind dissipated in ejecta?
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Summary:•UHECR spectrum extends at least beyond 100 EeV•Probably extragalactic & ‘light’ hadrons•Serious constraints on source physics and spatial distributions •Proposed astrophysical source models numerous•Common themes:
Strong, very fast shocks (relativistic)Strong shear (relativistic)Rapidly rotating, magnetized objects/relativistic winds
•All models require some ‘faith’ to get > ZeV, enough flux•New data (CR spectrum, isotropy, composition, & )
should trim/refine the list.
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The End
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Structure Shock Mach number distribution by upstream phase
Hot:T > 107 K
WHIM105 K< T < 107 K
‘External’shocks
Regions surroundingClusters containModerately strongShocks(unvirialized)
Hallman (UMN PhD thesis (2004))
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Energy Extracted by CRs Could be Substantial
Hallman (UMN PhD thesis (2004))
Triangles: Thermal
Squares: CRs(nonlinear DSAModel fromRyu etal 2003)
Shock dissipation nearClusters (R < 1 h-1 Mpc)
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Can Structure Shocks Accelerate UHECRs?
With standard diffusionassumptions (i.e, Bohm), DSA just too slow with likely fields to beat photopion losses above GZK
cTu
cr
s
g
320
1
23
20
Gauss7.2
1092
39
a
EeV
Z
E
K
TxB
Setting a < gives
or
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Quasi-Perpendicular Shocks Might Beat This (?)
If MHD turbulence is weak ( = rg >> rg)and B perp to shock normal, then, cross-field diffusioncontrols DSA (Jokipii, (ApJ, 313, 842 ( 1987)): perp (1/2) par, where < (c/us)
a ~ (1/ 2) a (Bohm) << a (Bohm)
Kang, Rachen & Biermann (MNRAS, 286, 257 (1998))
Additional constraints: diffusion along B (escape)Ostrowski & Siemieniec-Ozieblo (A&A 386, 829 (2002),
Or requiring rg < Rshock.Both basically return the Hillas constraint, soB » G (clusters) B » 100 nG (filaments)
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Turbulent, 2nd Order Acceleration
Very likely present, but generally slower than DSA
For strong Alfvenic turbulence, compared to strong shock DSA
a(2nd order) ~ (us/vA)2 a(DSA) » a(DSA)
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HiRes Collab ‘02
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‘Dead Quasars’
Boldt & Ghosh 1999Levinson 2000
•Quasars rare today• However, most galaxies host SMBH•‘Dead’ or ‘underfed’ AGNs•B & G estimate > ten 109 Msun SMBH within 50 Mpc•~ 2x10-5 Mpc-3; L ~ 1042 erg/sec
•Model: Extraction of rotational energyvia BZ-induced magnetic field: emf ~ 1021 V (109 Msun)•Curvature radiation reduces limit > order of magnitude
•Details not available