Neutrino Astronomy

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Neutrino flavor

Slide 47

Tau Transparency/Regeneration

ne and nµ are absorbed in the Earth via charged current interactions (muons range out)

Above ~100 TeV the Earth is opaque to ne & νµ.

But, the Earth never becomes completely opaque to nt

Due to the short t lifetime, t’s produced in nt charged-current interactions decay back into nt

Also, secondary ne & νµ. fluxes are produced in the tau decays.

Slide 48

Flavor Ratios

The ratio of flavors at the source is expected to be 0:2:1= nt : nm : ne

Since the distance to the source is >> than the oscillation length – any admixture at the source should wind up:

1:1:1= nt : nm : ne

when arriving at earth

What if that isn’t true?

Slide 49

Exotic neutrino properties if not 1:1:1

Neutrino decay (Beacom, Bell, Hooper, Pakvasa& Weiler)

CPT violation (Barenboim& Quigg)

Oscillation to steriles with very tiny delta δm2

(Crocker et al; Berezinskyet al.)

Pseudo-Dirac mixing (Beacom, Bell, Hooper, Learned, Pakvasa& Weiler)

3+1 or 2+2 models with sterile neutrinos (Dutta, Reno and Sarcevic)

Magnetic moment transitions (Enqvist, Keränen, Maalampi)

Varying mass neutrinos (Fardon, Nelson & Weiner; Hung & Pas)

Slide 50

Amanda-II

Amanda-B10

IceCube

Supernova Monitor

B10:

60% of Galaxy

A-II:

95% of Galaxy

IceCube:

up to LMC

Slide 51

Large Scale Neutrino Detectors

NESTOR

Pylos, Greece

ANTARES

La-Seyne-sur-Mer, France

BAIKAL

Russia

IceCube, South Pole, Antarctica

NEMO

Catania, Italy

See Talks in this Session

Slide 52

Radio Cherenkov Detectors

Rice Anita Salsa

Slide 53

Acoustic Detectors

SAUND (Study of Acoustic Underwater Neutrino Detection)

Slide 54

Conclusions

Now Soon Future

Amanda Cherenkov arrays ???

SK Radio Detectors

Neutrino Astronomy is just beginning to open a new window on the Universe!