Anisotropic pressure in brown dwarf stars

The dynamical nature of the fluid motion in very low-mass and brown dwarf stars indicates that the magnetic field has to be generated in these objects by dynamo action. Pressure in these stars is supported partially by non-relativistic degenerate electrons. It was established that the magnetic field can act on degenerate gas produces pressure anisotropy. Also anisotropy can be generated in rotating stars. Hence magnetic field and rotation may be considered as a source of anisotropy in such stars. This paper addresses the effect of anisotropy in the minimum mass of hydrogen burning and in brown dwarf stars. The results show that the minimum mass of the star needs to be increased to reach the stability condition due to the existence of pressure anisotropy and there was a change in the mass-radius relation for that stars.