Boundary Layer Self-Similar Solution for the Hot Radiative Accretion onto a Rapidly Spinning Neutron Star

Details Boundary Layer Self-Similar Solution for the Hot Radiative Accretion onto a Rapidly Spinning Neutron Star Boundary Layer Self-Similar Solution for the Hot Radiative Accretion onto a Rapidly Spinning Neutron Star

2004-06-16

arxiv.org/abs/astro-ph/0406377v1

Astrophys.J. 613 (2004) 506-511

Astronomy and Astrophysics

Astrophysics

14 pages, 1 figure. accepted for publication in ApJ

Scientific paper

10.1086/422990

We consider hot accretion onto a rapidly spinning neutron star (or any other compact object with a surface). A radiative hot settling flow has been discovered at low accretion rates in the early work by Medvedev & Narayan (2001) and analytical solution has been presented. It was shown later that this flow can match external medium smoothly, thus enforcing its physical feasibility. Here we complete the study of the global structure of such hot accretion by presenting the analytical solution for the boundary later, which forms between the bulk of the flow and the stellar surface. We confirm our results via full numerical solution of height-integrated two-temperature hydrodynamic equations.

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