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.
Institute for Space Studies Report Number X-644-62-78 (1962
- Pub Date:
- October 1962