Boundary layer on the surface of a neutron star
Abstract
In an attempt to model the accretion on to a neutron star in low-mass X-ray binaries, we present 2D hydrodynamical models of the gas flow in close vicinity of the stellar surface. First, we consider a gas pressure-dominated case, assuming that the star is non-rotating. For the stellar mass we take Mstar = 1.4 × 10-2Msolar and for the gas temperature T = 5 × 106 K. Our results are qualitatively different in the case of a realistic neutron star mass and a realistic gas temperature of T ~= 108 K, when the radiation pressure dominates. We show that to get the stationary solution in a latter case, the star most probably has to rotate with the considerable velocity.
- Publication:
-
Monthly Notices of the Royal Astronomical Society
- Pub Date:
- May 2008
- DOI:
- 10.1111/j.1365-2966.2008.13099.x
- arXiv:
- arXiv:0802.1663
- Bibcode:
- 2008MNRAS.386.1038B
- Keywords:
-
- accretion;
- accretion discs;
- hydrodynamics;
- stars: neutron;
- Astrophysics
- E-Print:
- 7 pages, 7 figures