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Conference Paper

Distortion of neutron stars with a toroidal magnetic field

MPS-Authors

Frieben,  Joachim
Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

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Rezzolla,  Luciano
Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

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1402.3258v2.pdf
(Preprint), 371KB

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Citation

Frieben, J., & Rezzolla, L. (2015). Distortion of neutron stars with a toroidal magnetic field. In Proceedings of the MG13 Meeting on General Relativity (pp. 2387-2389). World Scientific.


Cite as: https://hdl.handle.net/11858/00-001M-0000-0024-DCC1-7
Abstract
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.