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Evolution of newborn rapidly rotating magnetars: Effects of R-mode and fall-back accretion

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Wang,  Jieshuang
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

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Citation

Wang, J., & Dai, Z.-G. (2017). Evolution of newborn rapidly rotating magnetars: Effects of R-mode and fall-back accretion. Astrophysics & Astronomy, 603: A9. doi:10.1051/0004-6361/201629610.


Cite as: http://hdl.handle.net/21.11116/0000-0000-B627-7
Abstract
In this paper we investigate effects of the r-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 r-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 r-mode amplitude significantly. The maximum r-mode amplitude reaches an order of similar to 0.001 when the damping due to the growth of a toroidal magnetic field balances the growth of the r-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 r-mode amplitude is mainly due to the accretion torque. In this case, the maximum r-mode amplitude is of the order of similar to 10(-6)-10(-5).