Magnetorotational Instabilities and Pulsar Kick Velocities
arXiv:1507.04763 · doi:10.1016/j.newast.2015.07.004
Abstract
At the end of their birth process, neutron stars can be subject to a magnetorotational instability in which a conversion of kinetic energy of differential rotation into radiation and kinetic energies is expected to occur at the Alfvén timescale of few ms. This birth energy conversion predicts the observed large velocity of neutron stars if during the evolving of this instability the periods are of few ms and the magnetic fields reach values of G.
Accepted for publication in New Astronomy
References in corpus (6)
- The ATNF Pulsar Catalogue
- The McGill Magnetar Catalog
- Getting Its Kicks: A VLBA Parallax for the Hyperfast Pulsar B1508+55
- Evolution of magnetized, differentially rotating neutron stars: Simulations in full general relativity
- Multi-Dimensional Explorations in Supernova Theory
- Numerical Simulations of Equatorially-Asymmetric Magnetized Supernovae: Formation of Magnetars and Their Kicks