2009/08/07 by Shigenobu Hirose, Omer Blaes, Julian H. Krolik · 1 citation
Earth and Planetary Sciences · Physics and Astronomy · #Astrophysical Phenomena and Observations #Astrophysics #Astrophysics and Star Formation Studies #High-pressure geophysics and materials #Instability #Magnetohydrodynamics #Mechanics #Nuclear physics #Optics #Physics #Plasma #Radiation #Radiation pressure #Thermal #Thermodynamics #Turbulence #astro-ph.HE
paper · pdf · doi:10.1088/0004-637x/704/1/781
accepted for publication in The Astrophysical Journal
arxiv created 2009/08/07 · openalex publication_date 2009/09/25 · arxiv updated 2015/05/13 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/06
We present the results of a series of radiation MHD simulations of a local patch of an accretion disk, with a fixed vertical gravity profile but with different surface mass densities and a broad range of radiation to gas pressure ratios. Each simulation achieves a thermal equilibrium that lasts for many cooling times. After averaging over times that are long compared to a cooling time, we find that the vertically integrated stress is approximately proportional to the vertically averaged total thermal (gas plus radiation) pressure. We map out—for the first time on the basis of explicit physics—the thermal equilibrium relation between stress and surface density: the stress decreases (increases) with increasing surface mass density when the simulation is radiation (gas) pressure dominated. The dependence of stress on surface mass density in the radiation pressure dominated regime suggests the possibility of a Lightman–Eardley inflow instability, but global simulations or shearing box simulations with much wider radial boxes will be necessary to confirm this and determine its nonlinear behavior.