On the Solution Space of Differentially Rotating Neutron Stars in General Relativity

Details On the Solution Space of Differentially Rotating Neutron Stars in General Relativity On the Solution Space of Differentially Rotating Neutron Stars in General Relativity

2008-12-17

arxiv.org/abs/0812.3347v2

Astronomy and Astrophysics

Astrophysics

General Relativity and Quantum Cosmology

9 pages, 10 figures, version to be published in MNRAS ; no major changes with respect to v1: title, abstract and other things

Scientific paper

A highly accurate, multi-domain spectral code is used in order to construct sequences of general relativistic, differentially rotating neutron stars in axisymmetry and stationarity. For bodies with a spheroidal topology and a homogeneous or an N=1 polytropic equation of state, we investigate the solution space corresponding to broad ranges of degree of differential rotation and stellar densities. In particular, starting from static and spherical configurations, we analyse the changes of the corresponding surface shapes as the rate of rotation is increased. For a sufficiently weak degree of differential rotation, the sequences terminate at a mass-shedding limit, while for moderate and strong rates of differential rotation, they exhibit a continuous parametric transition to a regime of toroidal fluid bodies. In this article, we concentrate on the appearance of this transition, analyse in detail its occurrence and show its relevance for the calculation of astrophysical sequences. Moreover, we find that the solution space contains various types of spheroidal configurations, which were not considered in previous work, mainly due to numerical limitations.

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