Table of Contents
ISRN Astronomy and Astrophysics
Volume 2012, Article ID 420938, 14 pages
Research Article

Effect of Radiative Heat-Loss Function and Finite Larmor Radius Corrections on Jeans Instability of Viscous Thermally Conducting Self-Gravitating Astrophysical Plasma

1School of Studies in Physics, Vikram University, Madhya Pradesh, Ujjain 456010, India
2Department of Physics, Mahakal Institute of Technology, Madhya Pradesh, Ujjain 456664, India

Received 3 April 2012; Accepted 15 June 2012

Academic Editors: C. W. Engelbracht, A. Ferrari, F. Fraschetti, I. Goldman, and C. Meegan

Copyright © 2012 Sachin Kaothekar and R. K. Chhajlani. This is an open access article distributed under the Creative Commons Attribution License, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.


The effect of radiative heat-loss function and finite ion Larmor radius (FLR) corrections on the self-gravitational instability of infinite homogeneous viscous plasma has been investigated incorporating the effects of thermal conductivity and finite electrical resistivity for the formation of a star in astrophysical plasma. The general dispersion relation is derived using the normal mode analysis method with the help of relevant linearized perturbation equations of the problem. Furthermore the wave propagation along and perpendicular to the direction of external magnetic field has been discussed. Stability of the medium is discussed by applying Routh Hurwitz’s criterion. We find that the presence of radiative heat-loss function and thermal conductivity modify the fundamental Jeans criterion of gravitational instability into radiative instability criterion. From the curves we see that temperature dependent heat-loss function, FLR corrections and viscosity have stabilizing effect, while density dependent heat-loss function has destabilizing effect on the growth rate of self-gravitational instability. Our result shows that the FLR corrections and radiative heat-loss functions affect the star formation.