Evolution of newborn rapidly rotating magnetars: effects of r-mode and fall-back accretion
arXiv:1705.03579 · doi:10.1051/0004-6361/201629610
Abstract
In this paper we investigate effects of the -mode instability on a newborn rapidly-rotating magnetar with fall-back accretion. Such a magnetar could usually occur in core-collapse supernovae and gamma-ray bursts. We find that the magnetar's spin and -mode evolution are influenced by accretion. If the magnetar is sufficiently spun up to a few milliseconds, gravitational radiation leads to the growth of the -mode amplitude significantly. The maximum -mode amplitude reaches an order when the damping due to the growth of a toroidal magnetic field balances the growth of the -mode amplitude. If such a sufficiently spun-up magnetar was located at a distance less than 1\,Mpc, then gravitational waves would be detectable by the Einstein Telescope but would have an extremely low event rate. However, if the spin-up is insufficient, the growth of the -mode amplitude is mainly due to the accretion torque. In this case, the maximum -mode amplitude is of the order of .
7 pages, 3 figures, accepted for publication in A&A
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