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

Abstract

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.

14 pages, 1 figure. accepted for publication in ApJ

References in corpus (2)

• On the accretion luminosity of isolated neutron stars
• Self-Similar Hot Accretion onto a Spinning Neutron Star: Matching the Outer Boundary Conditions

Cited by in corpus (7)

• Modelling the behaviour of accretion flows in X-ray binaries
• On Hydromagnetic Stresses in Accretion Disk Boundary Layers
• Boundary layer on the surface of a neutron star
• A systematic study of the advection-dominated accretion flow for the origin of the X-ray emission in weakly magnetized low-level accreting neutron star
• The radiative efficiency of neutron stars at low-level accretion
• Hot accretion flow around neutron stars
• Two-temperature radiative hot accretion flow around neutron stars