1018eV Neutrinos associated with UHECR (>1019eV) sources

1
1018eV Neutrinos associated with UHECR (gt1019eV)
sources

• Zhuo Li (??)
• Peking University, Beijing
• Collaborators Eli Waxman Liming Song

Li Waxman, arXiv0711.4969
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Why EeV neutrino

• To directly identify CR sources
• Neutrino
• Pointing to the source
• Avoiding absorption
• 1018eV
• Primary gt1019eV

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HE Neutrinos from CR accelerators

• ?-production in accelerators
• acc. ps acc. es synchrotron/IC photons
• If all p energy converted to ? (in the source)
• Waxman-Bahcall Bound for sources optically thin
  to p

Waxman Bahcall 1999
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UHECR source acceleration
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GRB HE ns pg interaction

• p? m nm (10-8s)
• m? e ne nm (10-6s)

_
e?0.05 ep
eg ep0.2GeV2G2

• D-resonance
• eg1 MeV ? en1014eV.

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Spectral cutoff EM cooling

• For gt10PeV protons, the fraction of total energy
  loss
• Suppressed by pi/mu EM energy loss
• ?life??, tcool?1/?

en2n(en)
f?0.2
Waxman Bahcall 1997
1PeV
100TeV
Neutrino energy
No UHE neutrinos, how to identify UHECR sources?
Kashiti Waxman 2005 Rachen Meszaros 1998
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EeV neutrinos ?0-induced
en2?n
WB bound f?1
f?0.2
No cooling suppression 3 WB bound
Prompt 10sec
100TeV
1PeV
1EeV
en
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HE ?s from neutral ?0 production

• Processes

p0
g
CMB
EM cooling suppression
m
n
no cooling suppression
Li Waxman 2007b
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• Q1 suppressed by e- production?
• Q2 deflected by IGM field (hence delayed)?

CMB peak
?n???2
cross section ???-1, similar ? above ? threshold
e- thr.
?- thr.
?1019-20eV, ??/?e(3-10)
Li Waxman 2007b
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Q3 HE ?s escape from source?

• Attenuated by e- production in source
• low energy break
• KN suppression of cross section
• Strong synchrotron absorption below keV
• Conclusion gt10PeV photons dont suffer
  attenuation

dn/de
Li Waxman 2007b
1MeV
1keV
e
Li Waxman 2007a
Li Song 2004
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EeV neutrinos a new channel
en2?n
WB bound
1
0.2
20/km2yr 1km2 experiment
0.03
100TeV
1PeV
1EeV
en
n-g association (time/direction) directly
identify sources
Li Waxman 2007b
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• Coherence radio Cerenkov
• ANITA (balloon)
• ARIANNA (array)
• 1/yr expected

Barwick 2007