1. “Promises” of HE Neutrinos
David Eichler

2. The “dovecote” for HEN Theorists (circa 1979)
Accretion column, jet
Binary companion
target
Dense clouds
Dense clouds
SN ejecta
Winds
HE ion source
SN Remnants
AGN, etc.
Neutron Stars
Microquasars
Winds
GRB (not yet
understood)

3. Has anything changed?

4. Has anything changed?
Young neutron stars in dense supernova ejecta are now called “failed GRB”.

5. Has anything changed?
Shock acceleration dependability, efficiency generally accepted now, (though relativistic shocks may be less efficient, could be a major problem)

6. Has anything changed?
Shock acceleration dependability, efficiency generally accepted now, (though relativistic shocks may be less efficient, could be a major problem)
Note: spectrum goes as E-(2+p), so UHE energy flux for 1014eV^ (1020 eV) primaries goes as 10-5p (10-11p).

7. Has anything changed?
Shock acceleration dependability, efficiency generally accepted now, (though relativistic shocks may be less efficient, could be a major problem)
Collapsed star engines apparently blow out baryons (GRB afterglow)

8. Has anything changed?
Shock acceleration dependability, efficiency generally accepted now, (though relativistic shocks may be less efficient, could be a major problem)
Collapsed star engines apparently blow out baryons (GRB afterglow)
AGN detected [EGRET] to put out LEM=1048 erg/s or more in HE emission. [You can never limit Ltotal, because much of output of central engine could be unobservable (e.g. baryon kinetic energy), or transient.]

9. Has anything changed?
Shock acceleration dependability, efficiency generally accepted now, (though relativistic shocks may be less efficient, could be a major problem)
Collapsed star engines apparently blow out baryons (GRB afterglow)
AGN detected [EGRET] to put out 1048 erg/s or more in HE emission
UHE gamma ray astronomy providing good sanity check for energy budgets, acceleration efficiency

10. The Bad News for GRB Neutrinos:
They have lower fluences than AGN
Eichler 1994

11. There was, of course, bad nus on occasion, (Lande 1974, Cygnets, GZK cutoff violation…..).

12. The Good News for GRB:
The bad news was a generation ago

13. The Good News for GRB: The bad news was a generation ago
GRB teach us that baryons, outflow, particle acceleration can be generated by collapsed stellar remnants

14. The Good News for GRB: Why? The bad news was a generation ago
GRB teach us that baryons, outflow, particle acceleration can be generated by collapsed stellar remnants
We don’t see most GRB! Probably ~99.9% go unseen. So maybe the neutrinos will come from the other 99.9%
Why?

15. For a given energy output, Vmax = Rmax3ΔΩ α Ω-1/2
is enhanced by collimation.
If the universe were bigger, detected GRB would be, on average, even more collimated.
But…there may be a “quiet majority” of less collimated GRB or radiation fields from them that are much closer, and more relevant to HE neutrinos and gravitational waves.

16. kinematically softened photons at large viewing angles,
Because collimation enhances detectability, it overrepresents highly collimated, distant radiation.
Various types of uncollimated radiation –
scattered photons,
kinematically softened photons at large viewing angles,
gravitational waves,
neutrinos
may coincide with each other more often. Nearby events from the “quiet majority” may be waiting for us in coincidence from the relatively uncollimated forms of radiation.

17. Scattered photons from GRB?
GRB (SN 1998bw)
GRB
Smooth light curves, proximity, deviation from the Amati relation, all consistent with scattering off “slow” baryons.
Hard to soft evolution of light curve consistent with acceleration of scatterer

18. Lorentz transformation
Scattering increases solid angle, favors nearby sources
Lorentz transformation

19. Lorentz transformation
Scattering increases solid angle, favors nearby sources
Lorentz transformation
Anything with a back edge, (ejecta, plowed up wind material, pair fireball)

20. Scattering increases solid angle, favors nearby sources
Obs
Scattering increases solid angle, favors nearby sources

21. scattering
Scatterring always raises source above and/or to left Eichler and Mandal ‘09

22. Smooth light curves evidence for a light echo.

23. GRB

24. Smothered GRB
(DE and Levinson 1999)
If GRB scattered off x optical depths of scattering material, then there should be a lot more with different optical depth . For x>>10, GRB might be smothered, but you might detect neutrinos and possibly other stuff, e.g. adiabatically decelerated gamma rays (now known as dirty fireballs).
Smothering direction dependent, more general than “failed” GRB, which are very smothered.

25. GRB

26. Not the GRB. Adiabatically cooled gamma rays, or breakout flash?
GB explained as scattering off accelerating screen
Not the GRB. Adiabatically cooled gamma rays, or breakout flash?
Mandal and DE ‘09

27. Short hard GRB [SHB]
Wider viewable angle + acceleration by radiation pressure consistent with -
absence of giant envelope, galaxy type
closer distances
shorter duration
harder spectra
long, soft tails

28. Accelerating fireball

29. Accelerating fireball
Neutrinos?
GW?

30. So short GRB may have wider cone of detection that longer ones
So short GRB may have wider cone of detection that longer ones. But, X-ray tails of short bursts may have even wider cones of detection.

31. Long GRB Failure?
Most collapsars do not have magnetic fields of 1015 G. Energy release may be much slower, so central engine may fail to punch hole in host envelope.
Failed GRB may be much more frequent than successful ones (DE and Levinson ’99).

32. Conclusions
Gravitational waves, neutrinos, scattered gamma rays, and possibly X-ray tails more likely to coincide with each other than with (even) short GRB.
New concepts in wide angle X-ray cameras welcome (for X-ray tails, dirty fireballs, breakout flashes)
Most promising HE GRB neutrino sources may be smothered or failed GRB

33. Good luck to the brave experimentalists. You deserve it.
Conclusions
Good luck to the brave experimentalists. You deserve it.

34. (Levinson and Eichler 2004)
Top down neutrino production
(Levinson and Eichler 2004)
Sprinkle B field line-crossing neutrons into a pure Poynting flow, high G:
Wait for one to decay, get collisional avalanche with observer frame energy of G2.
Most burst energy radiated as neutrinos