Thin accretion disc with a corona in a central magnetic field |
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| Authors: | Fazeleh Khajenabi Mohsen Shadmehri Sami Dib |
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| Institution: | (1) School of Mathematical Sciences, University College Dublin, Belfield, Dublin 4, Ireland;(2) School of Mathematical Sciences, Dublin City University, Glasnevin, Dublin 9, Ireland;(3) Department of Physics, School of Science, Ferdowsi University, Mashhad, Iran;(4) Department of Physics, Faculty of Sciences, Lebanese University, El Hadath, Beirut, Lebanon;(5) Service d’Astrophysique, CEA/DSM/DAPNIA/SAp, CEA/Saclay, 91191 Gif-sur-Yvette Cedex, France |
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| Abstract: | 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. |
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| Keywords: | Accretion discs Stars: magnetic field Stars: neutron |
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