2014/02/28 by Joachim Frieben, Luciano Rezzolla
Physics and Astronomy · #astro-ph.SR #gr-qc
paper · pdf · doi:10.1142/9789814623995_0447
3 pages, 2 figures, to appear in the Proceedings of the 13th Marcel Grossmann Meeting held in Stockholm 1-7 July, 2012, based on arXiv:1207.4035. Updated to final published version
arxiv created 2014/09/12 · arxiv updated 2015/06/18
Models of rotating relativistic stars with a toroidal magnetic field have been computed for a sample of eight equations of state of cold dense matter. Non-rotating models admit important levels of magnetization and quadrupole distortion accompanied by a seemingly unlimited growth in size. Rotating models reach the mass-shedding limit at smaller angular velocities than in the non-magnetized case according to the larger circumferential equatorial radius induced by the magnetic field. Moreover, they can be classified as prolate-prolate, oblate-prolate, or oblate-oblate with respect to surface deformation and quadrupole distortion. Simple expressions for surface and quadrupole deformation are provided that are valid up to magnetar field strengths and rapid rotation.