Abstract—
Within the framework of Tsallis nonextensive statistics, the criteria for the Jeans gravitational instability are derived for a self-gravitating protoplanetary disk, whose substance consists of a mixture of a conducting ideal q-gas and modified radiation of a photon gas. The instability criteria are derived from the corresponding dispersion relations written for both neutral disk matter and magnetized plasma with modified blackbody radiation. The thermodynamics of a photon gas are constructed based on the nonextensive Tsallis quantum entropy, which depends on the deformation parameter. It is shown that blackbody q-radiation can stabilize the state of a nonextensive medium for a purely gaseous disk, and for an electrically conducting disk, the Jeans instability criterion is modified by the magnetic field and radiation pressure only in the transverse propagation mode of the disturbance wave.
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Notes
In the cited work, the kinetic theory was based on the Bhatnager–Gross–Krook (BGK) collision operator, which was generalized to an arbitrary parameter value q.
Bose created statistical mechanics for photon gas; Einstein developed it to describe massive particles.
Integration over dV often comes down to replacing dV by the total volume V of a homogeneous photon gas.
The calculation of integrals of this kind was carried out in (Kolesnichenko, 2020 \(J_{q}^{{(n)}} = - \frac{{15\Gamma (1 - q)}}{{{{\pi }^{4}}{{{(q - 1)}}^{n}}}}\sum\limits_{k = 0}^n {\left\{ {\frac{{(n - k)n!}}{{k!(n - k + 1)!}}\frac{{\Gamma \left[ {(1 - q)(n - k)} \right]}}{{\Gamma \left[ {(1 - q)(n - k + 1)} \right]}}} \right\}} .\)
In what follows, we will omit the index q for a number of hydrodynamic and thermodynamic variables.
The particular importance of the relationship (1 – β) for the theory of stellar structure was first pointed out by Eddington. In a famous passage from his book, The Internal Structure of Stars, Eddington linked this relationship to a “happening of the stars.”
When studying the disturbed states of self-gravitating cosmic material, one often has to deal with a variety of sound waves.
It should be noted that the linearized momentum equation requires that the velocity u be parallel to the wave vector ±k (see Landau and Lifshitz, 1964). Consequently, the velocities of liquid particles associated with adiabatic sound waves are parallel to the direction of wave propagation.
It is known that the problem of stability of a self-gravitating two-dimensional gas cloud, in principle, cannot be described within the framework of the two-dimensional approximation, since it is certainly highly unstable (see, for example, Fridman and Khoperskov, 2011). However, in the presence of a strong external gravitational field with a cylindrical geometry and with a generatrix along the axis of rotation of the cloud, it is possible to ensure its stability in the case when the angular velocity of rotation is sufficiently high. In this case, the structure of the preplanetary cloud along the axis of rotation will be determined exclusively by its self-gravity. Of course, this case is artificial, since in real astrophysical systems such cylindrical fields, even if they occur, are without embedded disks. At the same time, the consideration of such a self-gravitating gas disk embedded in a cylinder is of certain mathematical interest, since only in this case it is possible to single out the effects to which self-gravity leads in its pure form. Such models were considered in most of the classical works on astrophysical disks (see, for example, Goldreich and Lynden-Bell, 1965; Hunter, 1972; Toomre, 1964).
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The author is grateful to the Government of the Russian Federation and the Ministry of Higher Education and Science of the Russian Federation for support under the grant 075-15-2020-780 (N13.1902.21.0039).
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Kolesnichenko, A.V. Jeans Instability of a Protoplanetary Circular Disk Taking into Account the Magnetic Field and Radiation in Nonextensive Tsallis Kinetics. Sol Syst Res 55, 132–149 (2021). https://doi.org/10.1134/S0038094621020039
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DOI: https://doi.org/10.1134/S0038094621020039