Neutrino Astronomy

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R  1014 cm, T  3 x 103 seconds

R  1018 cm, T  3 x 1016 seconds

E  1051 – 1054 ergs

Shock variability is reflected in the complexity of the GRB time profile.

6 Hours

3 Days

Radio

Optical

-ray

X-ray

(2-10 keV)

Fireball Phenomenology & The Gamma-Ray Burst (GRB) Neutrino Connection

Progenitor

(Massive star)

Meszaros, P

Slide 26

Generic GRB Explosion Models

Slide 27

Lorentz Invariance Violation

Bounds on energy dependence of the speed of light can be used to place

constraints on the effective energy scale for quantum gravitational effects.

Dt ~ x(E/EQG)a L/c

E2-c2p2~E2x(E/EQG)a - This may be modified in some quantum gravity

models.

This has the important observational consequence that this will give

rise to energy dependent delays between arrival times of photons.

E2 = m2c4 +p2c2 - in the Lorentz invariant case,

The expected time delay is :

This may be measurable for very high energy photons/neutrinos coming

from large distances.

See Wed. Afternoon

Slide 28

Galactic Microquasars

See Talk Monday Morning

Slide 29

What About Dark Matter?

~85% of the matter in the Universe is Dark Matter

At most a few % of the matter is baryons

Most people believe that the lightest SUSY particle is a stable neutralino and is probably the dark matter

These are weakly interacting and heavy

Evidence of clustering

See Friday Afternoon Session on Dark Matter

Slide 30

Wimp Capture

Slide 31

Wimp Detection

Slide 32

Neutrino Astronomy Explores Extra Dimensions

100 x SM

GZK range

TeV-scale gravity increases PeV n-cross section

See Wednesday Afternoon Session

Slide 33

radiation

enveloping

black hole

black hole

p + g -> n + p+

~ cosmic ray + neutrino

-> p + p0

~ cosmic ray + gamma

Cosmic Neutrino Factory

Slide 34

W-B Bound

Slide 35

Evading the Bound

“Neutrino only” sources that are optically thick to proton photo-meson interactions and from which protons cannot escape.