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Neutrinos from Relativistic Outflows of Fast Spinning Magnetars

Published online by Cambridge University Press:  05 March 2013

Qinghuan Luo
Qinghuan Luo*
Affiliation:
School of Physics, University of Sydney, Sydney NSW 2006, Australia. Email: luo@physics.usyd.edu.au
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Abstract

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Pulsars may be born with a short rotation period of milliseconds with the magnetic field amplified through dynamo processes up to ∼1015–1016 G. Such millisecond magnetars spin down rapidly, emitting bursts of high-energy neutrinos and gamma rays. Specifically, acceleration of ions in both the polar gap (as in a normal pulsar) and the relativistic magnetar wind is considered. In both cases ions can be accelerated to ultra-high energies and these energetic ions can lead to production of high-energy neutrinos and gamma rays through interaction with thermal radiation from the hot neutron star or the heated inner boundary region of the stellar envelope as the result of the deposition of energy by the magnetar wind. The detectability of the neutrino flux by a kilometre-scale neutrino detector such as the planned IceCube neutrino observatory is discussed.

Keywords

neutrinosgamma rays: theoryradiation mechanisms: non-thermal
Type
ASA Conference 2004
Information
Publications of the Astronomical Society of Australia , Volume 22 , Issue 2 , 2005 , pp. 157 - 161
Copyright
Copyright © Astronomical Society of Australia 2005

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