Jet formation model from accretion disks of electron-ion-photon gas

Author: Nino Revazashvili
Keywords: Accretion, Accretion disks, Galaxies: jets, Galaxies:structure
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The problem of Astrophysical jet formation from relativistic accretion disks through the establishment of relativistic disk-powerful jet equilibrium structure is studied applying the Beltrami-Bernoulli equilibrium approach of [1], [2], [3]. Accretion disk is magnetized consisting of fully ionized relativistic electron-ion plasma and photon gas strongly coupled with electron gas due to Thompson Scattering. The main source of accretion is local viscosity, which we describe with generalized Shakura-Sunyaev α-turbulent dissipation model [4], where we have contributions of both the photon and ion gasses. We ignore the Hall term and the self-gravitation in the disk. For weakly magnetized disk we constructed the analytical self-similar solutions for the equilibrium relativistic disk-jet structure characteristic parameters and physical quantities [4]. The derived solutions can be used to analyze the astrophysical jets observed in binary systems during the star formation process linking the jet properties with the parameters of relativistic disks of electron-ion-photon gas. References : [1] Shatashvili, N. L., and Yoshida, Z., 2011 AIPCP, 1445 34-53; [2] Yoshida, Z., Shatashvili, N. L., 2012, arXiv:1210.3558; [3] Arshilava, E. Gogilashvili, M., Loladze, V., Jokhadze, I., Modrekiladze, B., Shatashvili, N. L., Tevzadze, A.G. 2019, J. High Energy Astrophysics 23, 6; [4] E. Katsadze , N. Revazashvili , N.L. Shatashvili ,„Jet formation model from accretion disks of electron-ion-photon gas“ Journal of High Energy Astrophysics V. 43 pp. 20-30 (2024) Present research was partially supported by Shota Rustaveli Georgian National Foundation Grant Project No. FR- 22-8273.