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Presupernovae as powerful neutrino sources

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Presupernovae as powerful neutrino sources

detectable by next neutrino experiments

M. Kutschera, A. Odrzywołek, M. Misiaszek

Ustroń 2009

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• Neutrino astrophysics group

• Institute of Physics, Jagellonian University, Kraków, Poland:

A.Odrzywołek, M. Misiaszek, M.K.

References to our papers: arXiv

Neutrino spectra available at

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• Research summary:

• Spectra of neutrinos from stars at late stages of thermonuclear burning (presupernovae) are found

• This allows us to predict counting rates in various neutrino detectors

• Presupernovae seem to be detectable by

next generation of neutrino detectors

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• Stars with initial mass (ZAMS) M>9M

sol

after red giant phase:

– ignite carbon

– develope iron core

– end life as core-collapse supernovae

– example: 15 M

sol

:

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Nearby candidate:

- Betelgeuse in ORION

constellation

- distance 130 pc

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• After carbon ignition neutrino-cooled stars

• Photon luminosity much less L<<L

ν

than neutrino luminosity.

-photon luminosity constant after carbon ignition

-neutrino luminosity grows by many orders!

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Strong temperature growth in the core

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Can neutrino experiments detect

presupernovae?

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• Pair annihilation dominant

• Antineutrino flux from pair annihilation crucial !

• Different than for the Sun (only neutrinos)

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High density – neutrino and antineutrino

spectra differ

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• Near the collapse:

– Total flux grows as L

ν

~T

c9

– Mean neutrino energy grows

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Predictions for various detectors

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• Range one day before collapse (various

detectors)

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Presupernova neutrinos vs geoneutrinos

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• Nuclear reactions produce more neutrinos ν

e

than pair annihilation

• More than 1000 nuclei must be included

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Weak nuclear reactions: neutrinos excess

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Comparison with

solar neutrinos

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REAL NEUTRINO ASTRONOMY

STARTS

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