Gravitational instability of rotating magnetized quantum anisotropic plasma

Abstract

The present problem deals with the study of gravitational (Jeans) instability of magnetized, rotating, anisotropic plasmas considering quantum effects. The basic equations of the considered system are constructed using combined Chew–Goldberger–Low (CGL) fluid model and quantum magnetohydrodynamic (QMHD) fluid model. A dispersion relation is obtained using the normal mode technique which is discussed for transverse and longitudinal modes of propagation. It is found that a rotating quantum plasma influences the gravitational mode in transverse propagation but not in longitudinal propagation. The presence of rotation decreases the critical wavenumber and it has a stabilizing effect on the Jeans instability criterion of magnetized quantum plasma in transverse propagation. The firehose instability is unaffected due to the presence of uniform rotation and quantum corrections. We observe from the numerical analysis that region of instability and critical Jeans wavenumber are both decreased due to the presence of uniform rotation. The stabilizing influence of uniform rotation is observed for magnetized, rotating, anisotropic plasmas in the presence of quantum correction. In the case of a longitudinal mode of propagation we found the Jeans instability criterion is not affected by rotation. The quantum diffraction term has a stabilizing effect on the growth rate of the Jeans instability when the wave propagates along the direction of the magnetic field.

Jeans gravitational instability of a magnetized rotating collision-less anisotropic plasma using generalized laws of double polytropy

“…For an infinite interstellar self-gravitating homogeneous cloud Jeans (1902) [1] obtained the criterion of gravitational instability, according to which the gas medium becomes unstable to vibrational perturbations of a wavelength exceeding a certain critical length, known as the Jeans length. In numerous subsequent publications, this result was extended to magnetized plasma both on the basis of the MHD equations for an ideal plasma (see, for example, [2][3][4][5][6][7][8][9][10][11][12][13][14][15][16][17][18]) and with the use of the single-fluid Chu-Goldberger-Low (CHL) hydromagnetic equations [19] with an aniso-Vol LIV (2022) 10.20948/mathmontis-2022-54-7 tropic pressure tensor using the double adiabatic equation of state [20][21][22][23][24][25][26][27]. In particular, various instabilities in interplanetary space plasma, for example, in the magnetosphere and planet plasma sphere, in stellar accretion disks, have been studied using the CHGL equations, taking into account the Hall current, pulsating viscous and radiative stress tensors, the effects of radiative heat conduction, magnetic field heterogeneity, etc.…”