1. Predictions of Ultra - High Energy Neutrino fluxes
Dmitry Semikoz
APC Paris

2. Overview: Introduction: high energy neutrinos
Neutrinos from UHECR protons, diffused neutrino flux
Neutrinos from astrophysical sources
Conclusion

3. INTRODUCTION

4. n's in AMANDA-II We can also say a few words about localy created nus
we have improvement compared to B10, better reco and energy measurement...sufficient statistics to do unfolding in statistically meaningfull way....
1 TeV

5. Why UHE neutrinos can exist?
Protons are attractive candidates to be accelerated in astrophysical objects up to highest energies E~1020 eV.
Neutrinos can be produced by protons in P+P -> pions or P+g-> pions reactions inside of astrophysical objects or in intergalactic space.
Neutrinos are produced by neutron decays: nuclei, proton-neutron conversion on CMB
Neutrinos can be produced by protons or nuclei during propagation.

6. Pion production n p
Conclusion: proton, photon and neutrino fluxes are connected in well-defined way. If we know one of them we can predict other ones:

7. Photons cascade down to low energies

8. Neutrinos from UHECR protons

9. The Greisen-Zatsepin-Kuzmin (GZK) effect
Nucleons can produce pions on the cosmic microwave background 
nucleon
pair production energy loss
pion production energy loss
pion production rate
-resonance
multi-pion production
sources must be in cosmological backyard
within Mpc from Earth
(compare to the Universe size ~ 5000 Mpc)

10. HiRes: cutoff in the spectrum
“GZK” Statistics 3
Expect 42.8 events
Observe 15 events
~ 5 s 9 1 2
Bergman (ICRC-2005)

11. Auger Energy Spectrum 2007 6s

12. Mixed composition model: less neutrinos due to nuclei
D.Allard, E.Parizot and A.Olinto, astro-ph/
problem: escape of the nuclei from the source; galactic Fe?

13. Protons can fit UHECR data: minimal model
V.Berezinsky , astro-ph/
problem: composition

15. Photo-pion production

16. Parameters which define diffuse neutrino flux
Proton spectrum from one source:
Distribution of maximum energy of sources:
Distribution of sources:

17. Theoretical predictions of neutrino fluxes
WB bound: 1/E2 protons; distribution of sources – AGN; analytical calculation of one point near 1019 eV.
MPR bound: 1/E protons; distribution of sources – AGN; numerical calculation for dependence on Emax
The g-ray bound: EGRET

18. Parameter degeneration
G.Gelmini, O.Kalashev and D.S., astro-ph/

19. EGRET: diffuse gamma-ray flux
The high energy gamma ray detector on the Compton Gamma Ray Observatory (20 MeV - ~20 GeV)

20. Contribution of UHECR to EGRET
GLAST
O.Kalashev , D.S. and G.Sigl, astro-ph/

21. Contribution UHECR to EGRET diffuse background for different a and m.

22. Low flux of neutrino
Z.Fodor et al, hep-ph/

23. Future detection of neutrinos from UHECR protons (2002)
AGN,1/E
/ EUSO
Old sources
1/E^2

24. Auger tau-neutrino limit 2007

25. Summary GZK neutrinos There is low bound E^2F(E) > 0.3 eV/cm^2/s/sr
One need in “good” energy resolution to figure out the shape of the flux
One do not need in angular resolution
Search for individual sources at highest energies is hopeless

26. Neutrinos from astrophysical sources

27. TeV gamma-sources
Pulsars
and PWN
SNRs
GRBs
AGNs

28. Problem I with TeV sources
In order TeV blazars be a neutrino sources:
= spg ng R>>1
= sgg ng R <<1
spg = 6x10-28cm2 while sgg = 6.65 x 10-25cm2
CONTRADICTION!!!
Way out – production at different place/time or in p-p reactions.

29. Problem II with TeV sources
Any part of TeV gamma’s can be produced by electrons
One need to explain all low energy emission radio-to-X-ray in hadronic models: usually requires to introduce electrons anyway.
For individual source one can spread energy in gamma-rays on larger angle –neutrino flux can be enhanced. Price – few neutrino sources as compared to gamma-rays

30. Neutrino production in AGN core
A.Neronov & D.S., hep-ph/

31. Example 1: blazars. Photon background in AGN core
Energy scale
Eg= 0.1 – 10 eV
Time variability
t ~ few days or
R = 1016cm
Model: hot thermal radiation.
T=10 eV
T=1 eV

32. Photo-pion production

33. Neutrino spectrum for various proton spectra and backgrounds
Atm.
flux
1/E
E~1018eV
1/E2
AMANDA II
ANTARES
T=1 eV
T=10 eV
1/E2

34. Example 2: Variable TeV emission from binary LS I +61 303
Ten points at equal phase intervals from F = 0 to F = 0.9,
with MAGIC observations (where available) on the right.
The periastron is at F = 0.2.
MAGIC Collaboration, Science 312: ,2006
F=( )*10-12 /cm2/s/TeV .

35. Electromagnetic model of binary LS I +61 303
Zdziarski et al, arXiv:

36. Neutrino emission from p+p process
Diego F. Torres, Francis Halzen , Astropart.Phys.27: ,2007.
If F_nu=F_gamma events /2.5 background /year

37. Other galactic sources
Galactic cosmic rays (talk by A.Taylor)
Milagro sources (talk by A.Kappes)

38. Summary neutrinos from point sources
P-P reaction can give a hope to follow galactic TeV sources (example: binary systems)
GLAST: May 2008! Galactic and extragalactic candidates at multi-GeV!
One need in “as good as possible” angular resolution to suppress background AND to find out which source is real one.
It would be nice to have good energy resolution.

39. Neutrinos from Galactic Supernova

40. Possible neutrino signals from Galactic SN in km^3 detector
Prompt neutrino signal in 1-50 MeV energies.
1-10 sec after SN burst/Strong signal in each optical module / SN 1987A signal
events with E> 1TeV in hours after burst. Shock front reached surface and became colisionless.
Duration t ~ 1 hour / Waxman & Loeb 2001
SN shock interact with pre-SN wind and interstelar medium events with E>1 TeV in km^3 detector
From 10 days till 1 year /Berezinsky & Ptuskin 1989

41. Supernova Monitor Amanda-II B10: 60% of Galaxy A-II: 95% of Galaxy
IceCube:
up to LMC
Amanda-B10
sec
Count rates
IceCube

42. Pointing to Galactic SN
AMANDA II can see 5-20 events with E> 1TeV. For AMANDA II angular resolution 2o of each event. Pointing to SN direction is possible with resolution ~0.5o
For ANTARES pointing is up to 0.1o .
Compare to SuperKamiokande 8o now and 3.5o
with gadolinium. HyperKamiokande ~0.6o

43. Detection of Galactic SN from ‘wrong side’ by km^3 detector
Atmospheric muons 5*1010/year or
300/hour/(1o)2
Signal 200 events, besides energy cut TeV.
Angular resolution 0.8o for each event or less then 0.1o for SN signal !!!
(A.Digle, M.Kachelriess, G.Raffelt, D.S. and R.Tomas, hep-ph/ )

44. Conclusions
All top-down and exotic models are not needed anymore for UHECR data. Bad news for neutrinos: no high fluxes at high energies.
Secondary neutrino flux from UHECR protons can be detected by km^3 experiments. Situation will clear up in 1-2 years after input of GLAST and new results from AUGER.
Neutrino flux from different kind of astrophysical sources can be detected by km^3 neutrino telescopes. However relation of neutrino fluxes to gamma-ray fluxes strongly model dependent.