Models for Stars of Very Low Mass

Completely convective models have been constructed for stars of masses 0.09, 0.08, 0.07, 0.06, 0.05 and 0.04 (solar units), taking into account the non-relativistic degeneracy of the stellar material. The properties of these models are presented in tabular form and in the form of graphs. It is shown that there is a lower limit to the mass of a main sequence star. The stars with mass less than this limit become completely degenerate stars or "black" dwarfs as a consequence of the gravitational contraction and therefore they never go through the normal stellar evolution.