Radiative condensation instability in partially ionized dusty plasma with polarization force

Abstract

This paper studies the effect of polarization force on the radiative condensation (RC) instability of a partially ionized dusty medium both in the presence and absence of self-gravitation. The temperature and density dependent heat loss function is considered in the process of heating and radiative cooling. The linear-perturbation analysis is used to derive general dispersion relation and criteria for both the Jeans and RC instability. The condition of Jeans instability is modified due to the RC, polarization force, magnetic field and dust thermal speed, whereas in the case of RC instability the instability criterion is modified due to the presence of dust thermal speed, magnetic field and polarization force. The effects of various parameters have been numerically estimated on RC instability. It is clear from figure that the presence of polarization parameter and density dependent heat-loss function destabilize the system while the presence of temperature dependent heat-loss function, dust neutral collision frequency and ratio of neutral dust density stabilize the system. These findings are relevant for many areas of space and laboratory plasma research prime examples being the formation of dense molecular clouds in interstellar and intergalactic medium, condensations in planetary nebulae and in laboratory plasmas like tokamak edge plasma.

Low frequency waves and instability in magnetized radiative dusty plasma

“…The dispersion relation (8)shows the electrostatic dust wave in the parallel mode while propagating in radiative self-gravitating plasma with the combined effect of polarization force, charge gradient force and radiative electrons. The influence of the magnetic field vanishes so radiative gravitating viscous mode is independent of the magnetic field.…”

“…The influence of the magnetic field vanishes so radiative gravitating viscous mode is independent of the magnetic field. If the system is considered non viscous then the expression (8) gives the radiative gravitating mode and the roots of the Eq. (8) becomes…”

“…If the critical mass is greater than the mass of the cloudthen the collapse does not take place due to self-gravitation, but the structure formation process is fastened by radiative cooling [5].Gilden [6] has discussed about radiative effect and thermal instability in the study of small scale structure formation. Kopp and Shchekinov [7]analysed the radiative effect in multi-fluid dusty plasma.The effect of polarization, effects of radiative coolingof electronand self-gravitation have been done by Sharma and Jain [8] to study instability of partially ionized dusty plasma. These works of radiative condensation and self-gravitation have considered the charge to remain constant on the dust particles.…”

Transverse Thermal Instability of Radiative Plasma with FLR Corrections for Star Formation in ISM

“…Certainly, when the gravitational power of originally uniform plasma is comparatively tiny the solar eminences (Tandberg-Hanssen [3]; Priest [4]) and numerous kinds of interstellar clouds (Spitzer [5]; Hollenbach & Thronson [6]; & Burton et al [7]) are structured because of the procedure of thermal strengthening. Thermal unsteadiness has been studied by several investigators for more than seven decades in astrophysical objects and plasma physics applications (Aggarwal and Talwar [8]; Bora and Talwar [9]; Fukue & Kamaya [10]; Prajapati et al [11]; Kaothekar et al [12]; Sharma and Jain [13]; Prajapati et al [14]). More recently Kaothekar [15] has discussed the thermal instability of partially ionized viscous plasma with Hall effect FLR corrections flowing through porous medium.…”

Impacts of Rotation Radiative Heat-loss Functions Porosity with FLR Corrections on Transverse Thermal Instability of Finitely Conducting Plasma in Interstellar Medium (ISM)

“…Indeed, when the gravitational energy of initially homogeneous plasma is relatively small, the solar prominences [Tandberg-Hanssen (1974); Priest (1989)] and many types of interstellar clouds [Spitzer (1978); Hollenbach & Thronson (1987); & Burton et al (1992)] are formed by the process of thermal condensation. Thermal instability has been explored by numerous researchers for more than seven decades in astrophysical objects and plasma physics applications [Aggarwal & Talwar (1969); Bora & Talwar (1993); Fukue & Kamaya (2007); Prajapati et al (2010); ; Sharma & Jain (2016); Prajapati et al (2016)]. Kaothekar (2018) has examined the thermal instability of partially ionized viscous plasma with Hall effect FLR corrections flowing through porous medium.…”