1999/09/30 by G. E. Brown, Chang‐Hwan Lee, C. -H. Lee +2 · 2 citations
Earth and Planetary Sciences · Physics and Astronomy · #Accretion (finance) #Accretion disc #Advection #Angular momentum #Astronomy #Astrophysical Phenomena and Observations #Astrophysics #Classical mechanics #Common envelope #Envelope (radar) #High-pressure geophysics and materials #Laser-Plasma Interactions and Diagnostics #Neutron star #Physics #Stars #Telecommunications #White dwarf #astro-ph
paper · pdf · doi:10.1086/309454
6 pages, ApJ, submitted
arxiv created 2000/04/24 · openalex publication_date 2000/10/01 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/06
In this paper we study the accretion disk that arises in hypercritical accretion of ~ 10 8 M Edd onto a neutron star while it is in common envelope evolution with a massive companion. Such a study was carried out by Chevalier, who had earlier suggested that the neutron star would go into a black hole in common envelope evolution. In his later study he found that the accretion could possibly be held up by angular momentum. In order to raise the temperature high enough that the disk might cool by neutrino emission, Chevalier found a small value of the α-parameter, where the kinematic coefficient of shear viscosity is ν = α c s H , with c s the velocity of sound and H the disk height; namely, α ~ 10 -6 was necessary for gas pressure to dominate. He also considered results with higher values of α, pointing out that radiation pressure would then predominate. With these larger α-values, the temperatures of the accreting material are much lower, ≳0.35 MeV. The result is that neutrino cooling during the flow is negligible, satisfying very well the advection-dominating conditions. The low temperature of the accreting material means that it cannot get rid of its energy rapidly by neutrino emission, so it piles up, pushing its way through the accretion disk. An accretion shock is formed, far beyond the neutron star, at a radius ≲10 8 cm, much as in the earlier spherically symmetric calculation, but in rotation. Two-dimensional numerical simulation shows that an accretion disk is reformed inside of the accretion shock, allowing matter to accrete onto the neutron star with pressure high enough so that neutrinos can carry off the energy.