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Cosmic Rays from Pair-Instability Supernova Remnants

Foss, Marie Kristine
Master thesis
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10485_FULLTEXT.pdf (2.423Mb)
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http://hdl.handle.net/11250/2352040
Utgivelsesdato
2015
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  • Institutt for fysikk [2148]
Sammendrag
Pair-instability supernovae are the most energetic thermonuclear explosions in the

Universe, up to 100 times more energetic than type Ia supernovae. Around redshift

z > 6 approximately one out of ten supernovae was a pair-instability supernova, in

the local universe, however, this number is drastically reduced to less than one out

of ten thousand. In this thesis we look at progenitors both among the first generation

of stars and in the local universe. We determine the dynamical evolution of the

supernova blast wave propagating through the interstellar medium. The maximum

energy a cosmic ray proton can be accelerated to in the supernova remnant is then

found to be 4e15 eV, for a mean magnetic field of 100 μG parallel to the shock

front. Lastly, the proton and neutrino flux for a Pop III pair-instability supernova

is estimated. The diffuse neutrino flux for PI SNe is found to be a sub-dominant

contribution to the observed flux.
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