Cosmological supernovae as neutrino and gravitational wave sources
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: arXivNeutrino 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>9Msol
after red giant phase:– ignite carbon– develope iron core – end life as core-collapse supernovae– example: 15 Msol :
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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<<Lν
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 Lν ~Tc
9
– 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 νe
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