A note on stellar ionization

In this paper, we examine the thermal ionization in the core of a main-sequence stable star with the assumption that the main-sequence stellar core behaves like an ideal 3-Dimensional (D) Fermi gas. This assumption is based on the fact that the stellar core persists as a region of very high temperature, typically in a range between 15 x 10(6) K and density near 150 gcm(-3), like that of our Sun where the classical gas description fails and Fermi-Dirac (F-D) distribution become important. Finally, we compare our ionization equation with Saha's thermal ionization equation based on classical Maxwell-Boltzmann (M-B) distribution. The mathematical analysis provides us with the result that the ionization fraction is proportional to the probability-distribution function and also exponentially proportional to the Fermi energy and has volume dependency under the 3-D ideal Fermi gas consideration, thus inducing an extensive nature for the equation of state.