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Power distributions for self-gravitating astrophysical systems based on nonextensive Tsallis kinetics

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Abstract

The long-time development of self-gravitating gaseous astrophysical systems (in particular, the evolution of the protoplanet accretion disk) is mainly determined by relatively fast processes of the collision relaxation of particles. However, slower dynamical processes related to force (Newton or Coulomb) interactions between particles should be included (as q-collisions) in the nonextensive kinetic theory as well. In the present paper, we propose a procedure to include the Newton self-gravity potential and the centrifugal potential in the near-equilibrium power-like q-distribution in the phase space, obtained (in the framework of nonextensive statistics) by means of the modified Boltzmann equation averaged with respect to an unnormalized distribution. We show that if the power distribution satisfies the stationary q-kinetic equation, then the said equation imposes clear restrictions on the character of the long-term force field and on the possible dependence of hydrodynamic parameters of the coordinates: it determines those parameters uniquely. We provide a thermodynamic stability criterion for the equilibrium of the nonextensive system. The results allow us to simulate the evolution of gaseous astrophysical systems (in particular, the gravitational stability of rotating protoplanet accretion disks) more adequately.

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  1. Keldysh Institute of Applied Mathematics, Russian Academy of Sciences, Moscow, Russia

    A. V. Kolesnichenko

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Original Russian Text © A.V. Kolesnichenko, 2017, published in Astronomicheskii Vestnik, 2017, Vol. 51, No. 2, pp. 142–160.

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Kolesnichenko, A.V. Power distributions for self-gravitating astrophysical systems based on nonextensive Tsallis kinetics. Sol Syst Res 51, 127–144 (2017). https://doi.org/10.1134/S0038094617020046

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