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Thermal Ionization in Stellar Core Based on Ideal Fermi Gas Model

by Shiladittya Debnath

Submission summary

As Contributors: Shiladittya Debnath
Preprint link: scipost_202103_00004v1
Date submitted: 2021-03-03 15:04
Submitted by: Debnath, Shiladittya
Submitted to: SciPost Astronomy Core
Academic field: Astronomy
  • Mathematical Physics
  • Solar and Stellar Astrophysics
Approach: Theoretical


This paper examines the thermal ionization in the core of a main-sequence stable star, with an assumption that the main-sequence stellar core behaves like an ideal 3-Dimensional (D) Fermi gas. This assumption has been based on the fact that the stellar core persists as a region of very high temperature, typically in a range between 15×〖10〗^6 K and density near 150 g cm^(-3), like that of our Sun where the classical gas description fails and Fermi-Dirac (F-D) distribution becomes important. Finally we compare our ionization equation with the Saha’s thermal ionization equation based on classical Maxwell-Boltzmann (M-B) distribution. The mathematical calculation provides us with the result that the ionization fraction is exponentially proportional to the Fermi energy and has volume dependency, under the 3-D ideal Fermi gas consideration.

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Submission scipost_202103_00004v1 on 3 March 2021

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