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arXiv · 0807.0267

Non-thermal neutrinos from supernovae leaving a magnetar

Shunsaku Horiuchi·Yudai Suwa·Hajime Takami·Shin'ichiro Ando·Katsuhiko Sato
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Abstract

Under the fossil field hypothesis of the origin of magnetar magnetic fields, the magnetar inherits its magnetic field from its progenitor. We show that during the supernova of such a progenitor, protons may be accelerated to \sim 10^4 GeV as the supernova shock propagates in the magnetic stellar envelope. Inelastic nuclear collisions of these protons produce a flash of high-energy neutrinos arriving a few hours after thermal (10 MeV) neutrinos. The neutrino flash is characterized by energies up to O(100) GeV and durations seconds to hours, depending on the progenitor: those from smaller Type Ibc progenitors are typically shorter in duration and reach higher energies compared to those from larger Type II progenitors. A Galactic Type Ib supernova leaving behind a magnetar remnant will yield up to \sim 160 neutrino induced muon events in Super-Kamiokande, and up to \sim 7000 in a km^3 class detector such as IceCube, providing a means of probing supernova models and the presence of strong magnetic fields in the stellar envelope.

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Shunsaku Horiuchi, Yudai Suwa, Hajime Takami, Shin'ichiro Ando, Katsuhiko Sato. 2008-11-14. Non-thermal neutrinos from supernovae leaving a magnetar. https://doi.org/10.1111/j.1365-2966.2008.14000.x

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