A mathematical solution for the formation of halo

The behaviour of dense astrophysical systems can be described by the magnetohydrodynamic equations involving gravitational potential. In this paper the magnetohydrodynamic equations are solved in the wave form and a general dispersion relation have been obtained. This dispersion relation has been used with simplifying assumptions, plausible for special regions of the system and results obtained have been shown to be able to interpret the property of the gas in those special regions. For example, a region at a large distance from the centre of the system — i.e.,r — is considered. The analysis indicates that instability exists at such a large distance though it is assumed that the region is homogeneous. This explains the formation of corona, envelope of supergiant or galactic halo.