Optically thin outbursts of rotating neutron stars can not be spherical
Abstract
We investigate three-dimensional relativistic trajectories of test particles in the spacetime of a slowly rotating compact star, under the combined influence of gravity and a strong, near-Eddington radiation field. While in the static case a spherically symmetric shell of matter suspended above the stellar surface can be formed at the location of radial equilibrium of effective forces, the same is not true for a rotating star. In the latter case the symmetry is broken by the interplay between motion in the non-static spacetime and the influence of strong radiation drag forces, pushing particles towards the equatorial plane. As a result an expanding spherical shell of matter ejected from the neutron star surface collapses on a short timescale into a single stable equatorial ring supported by radiation. These findings have implications for the geometry of optically thin outflows during luminous neutron star bursts.
Keywords
Cite
@article{arxiv.1907.11268,
title = {Optically thin outbursts of rotating neutron stars can not be spherical},
author = {Maciek Wielgus},
journal= {arXiv preprint arXiv:1907.11268},
year = {2019}
}
Comments
6 pages, 4 figures, accepted in MNRAS