http://arxiv.org/abs/1402.3258
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 accompanied by a seemingly unlimited growth in size and quadrupole distortion. Rotating models reach the mass-shedding limit at smaller angular velocities than in the non-magnetized case corresponding to the larger circumferential equatorial radius induced by the magnetic field. Moreover, they can be classified as prolate-prolate, prolate-oblate, or oblate-oblate with respect to quadrupole distortion and surface deformation. Simple expressions for surface and quadrupole deformation are provided that are valid up to magnetar field strengths and rapid rotation.
J. Frieben and L. Rezzolla
Tue, 18 Feb 14
49/72
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