Jeans anisotropic instability

Цинцадзе, Н. Л.; Rozina, Ch.; Ruby, R.; Tsintsadze, Levan N.

doi:10.1063/1.5029517

Cited by 12 publications

(14 citation statements)

References 37 publications

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“…Here, υ jα is the collisional frequency of particle α with j and u α , u j are their relative velocities respectively. We note here that when collisions between particles are very frequent (Tsintsadze et al 2018) the velocities of different plasma species must in fact be almost equal. It is quite evident from (2.1)-(2.8) that, if υ ei , υ eN and υ iN are significantly large, the frictional forces can be balanced by other terms only if the relative velocities of different species, u i − u e , u N − u e and u N − u i are small i.e.…”

Section: Basic Formalismmentioning

confidence: 81%

“…Here, we suppose that the neutron-electron collision frequency ν Ne is comparatively small. It was shown in Tsintsadze et al (2018) that in the presence of a quantized magnetic pressure, the plasma becomes anisotropic, and the associated momentum equations in the directions perpendicular and parallel to the applied superstrong magnetic field are respectively dp…”

Section: Basic Formalismmentioning

confidence: 99%

“…To show that nonlinear stationary waves can be formed in the dispersive pulsar atmosphere, we shall follow the method presented in Whitham (1974), Landau & Lifshitz (1987), Tsintsadze, Hussain & Murtaza (2011) and Tsintsadze et al (2018). For this purpose, in order to consider the x-dimensional propagation of fast magnetosonic waves travelling across the quantized magnetic field, let us re-write equations (2.2), (3.2), (3.5) respectively as…”

Section: Solitary Fast Magnetosonic Waves In a Weakly Dispersive Pulsarmentioning

confidence: 99%

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Magnetic field quantization in pulsars

2020

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Magnetic field quantization is an important issue for degenerate environments such as neutron stars, radio pulsars and magnetars etc., due to the fact that these stars have a magnetic field higher than the quantum critical field strength of the order of $4.4\times 10^{13}~\text{G}$ , accordingly, the cyclotron energy may be equal to or even much more than the Fermi energy of degenerate particles. We shall formulate here the exotic physics of strongly magnetized neutron stars, known as pulsars, specifically focusing on the outcomes of the quantized magnetic pressure. In this scenario, while following the modified quantum hydrodynamic model, we shall investigate both linear and nonlinear fast magnetosonic waves in a strongly magnetized, weakly ionized degenerate plasma consisting of neutrons and an electron–ion plasma in the atmosphere of a pulsar. Here, linear analysis depicts that sufficiently long, fast magnetosonic waves may exist in a weakly dispersive pulsar having finite phase speed at cutoff. To investigate one-dimensional nonlinear fast magnetosonic waves, a neutron density expression as a function of both the electron magnetic and neutron degenerate pressures, is derived with the aid of Riemann’s wave solution. Consequently, a modified Korteweg–de Vries equation is derived, having a rarefractive solitary wave solution. It is found that the basic properties such as amplitude, width and phase speed of the fast magnetoacoustic waves are significantly altered by the electron magnetic and the neutron degenerate pressures. The results of this theoretical investigation may be useful for understanding the formation and features of the solitary structures in astrophysical compact objects such as pulsars, magnetars and white dwarfs etc.

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Section: Basic Formalismmentioning

confidence: 81%

Section: Basic Formalismmentioning

confidence: 99%

Section: Solitary Fast Magnetosonic Waves In a Weakly Dispersive Pulsarmentioning

confidence: 99%

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Magnetic field quantization in pulsars

2020

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“…(2008) and this same group later included anisotropic effects (Tsintsadze et al. 2018). Interestingly, most of the work encountered in the literature addresses gravitational collapse as the main cause of contraction of astrophysical objects due to the increased gravity among dense and massive particles, while the mechanism of gravitational collapse due to surface oscillations was only pointed out recently (Rozina et al.…”

Section: Introductionmentioning

confidence: 99%

Surface waves on the inhomogeneous interface between radiative electron–ion plasma and vacuum

et al. 2021

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The impact of temperature inhomogeneity, surface charge and surface mass densities on the stability analysis of charged surface waves at the interface between dense, incompressible, radiative, self-gravitating magnetized electron–ion plasma and vacuum is investigated. For such an incompressible plasma system, the temperature inhomogeneity is governed by an energy balance equation. Adopting the one-fluid magnetohydrodynamic (MHD) approximation, a general dispersion relation is obtained for capillary surface waves, which takes into account gravitational, radiative and magnetic field effects. The dispersion relation is analysed to obtain the conditions under which the plasma–vacuum interface may become unstable. In the absence of electromagnetic (EM) pressure, astrophysical objects undergo gravitational collapse through Jeans surface oscillations in contrast to the usual central contraction of massive objects due to enhanced gravity. EM radiation does not affect the dispersion relation much, but actually tends to stabilize the Jeans surface instability. In certain particular cases, pure gravitational radiation may propagate on the plasma vacuum interface. The growth rate of radiative dissipative instability is obtained in terms of the wavevector. Our theoretical model of the Jeans surface instability is applicable in astrophysical environments and also in laboratory plasmas.

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“…Relying on the density and mass of the dusty grain, the electrostatic forces on the dusty grain become comparable to the gravitational forces, thus introducing the concept of the gravitational or Jeans instability. In this context, a huge amount of work is devoted to investigating the influence of different aspects of the Jeans instability such as the influence of thermal radiation (Tsintsadze et al 2008), quantized magnetic pressure (Tsintsadze et al 2018), degree of ionization (Shukla & Stenflo 2006), fluid viscosity (Mamun & Shukla 2000), rotation (Janaki, Chakrabarti & Banerjee 2011), effect of magnetic fields (Goldreich & Lynden-Bell 1965) and many other parameters that significantly influence the Jeans criterion. The importance of the self-gravitating, magnetized gravitational instability in the case of an astronomical plasma was discussed in Chandrashekhar (1961).…”

Section: Introductionmentioning

confidence: 99%

Gravitating–radiative magnetohydrodynamic surface waves

et al. 2020

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Radiative-magnetohydrodynamic (RMHD) equations along with a full set of Maxwell's equations are followed to formulate the charged surface waves at the interface of an incompressible, radiative, magnetized dusty plasma and vacuum, while assuming that the characteristic wave frequency is much smaller than the ion gyrofrequency, having an equilibrium background state. It is found that the separation of charges on the surface is followed by thermal motion, which further leads to a negative pressure gradient normal to the surface, hence the plasma–vacuum interface is under tension due to two different types of oppositely directed pressures. The dusty plasma RMHD set of equations admits a linear dispersion relation of surface Jeans instability of an incompressible dusty plasma, which exhibits a strong coupling between the electron surface charge and dust surface mass densities and we conclude that the surface densities of both electrons and dust as well as the dust inertia play major roles in the gravitational collapse of the surface of astrophysical objects such as stars, galaxies etc. Further, the growth rate of radiative surface waves is found to be function of both the temperature inhomogeneity, appearing due to thermal radiation heat flux, as well as the thermal radiation pressure. The present findings of charged surface waves may seek application at the astroscales.

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Jeans anisotropic instability

Cited by 12 publications

References 37 publications

Magnetic field quantization in pulsars

Magnetic field quantization in pulsars

Surface waves on the inhomogeneous interface between radiative electron–ion plasma and vacuum

Gravitating–radiative magnetohydrodynamic surface waves

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