2008/02/15 by Fazeleh Khajenabi, Mohsen Shadmehri, Sami Dib
Physics and Astronomy · #Accretion (finance) #Angular momentum #Astrophysical Phenomena and Observations #Astrophysics #Astrophysics and Star Formation Studies #Classical mechanics #Corona (planetary geology) #Corona discharge #Corona ring #Coronal mass ejection #Intermediate polar #Magnetic field #Magnetic pressure #Magnetization #Mechanics #Physics #Solar wind #Stars #Stellar magnetic field #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1007/s10509-008-9766-y
published as Astrophys.Space Sci.314:251-260,2008 · Accepted for publication in Astrophysics & Space Science
arxiv created 2008/02/15 · openalex publication_date 2008/02/28 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We study the steady-state structure of an accretion disc with a corona surrounding a central, rotating, magnetized star. We assume that the magneto-rotational instability is the dominant mechanism of angular momentum transport inside the disc and is responsible for producing magnetic tubes above the disc. In our model, a fraction of the dissipated energy inside the disc is transported to the corona via these magnetic tubes. This energy exchange from the disc to the corona which depends on the disc physical properties is modified because of the magnetic interaction between the stellar magnetic field and the accretion disc. According to our fully analytical solutions for such a system, the existence of a corona not only increases the surface density but reduces the temperature of the accretion disc. Also, the presence of a corona enhances the ratio of gas pressure to the total pressure. Our solutions show that when the strength of the magnetic field of the central neutron star is large or the star is rotating fast enough, profiles of the physical variables of the disc significantly modify due to the existence of a corona.