Non-thermal neutrinos from supernovae leaving a magnetar

Details Non-thermal neutrinos from supernovae leaving a magnetar Non-thermal neutrinos from supernovae leaving a magnetar

2008-07-02

arxiv.org/abs/0807.0267v2

Mon.Not.Roy.Astron.Soc.391:1893-1899,2008

Astronomy and Astrophysics

Astrophysics

8 pages, 1 figure, added 1 section and references

Scientific paper

10.1111/j.1365-2966.2008.14000.x

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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