Stellar critical parameters in the uniform density approximation
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arXiv
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| Format: | Preprint |
| Published: |
2025
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| _version_ | 1866914138828046336 |
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| author | Bisnovatyi-Kogan, G. S. Patraman, E. A. |
| author_facet | Bisnovatyi-Kogan, G. S. Patraman, E. A. |
| contents | Stellar models are calculated in the approximation of a uniform density distribution. Variational method was used for determination of the boundary of a stability loss, for stellar masses in the range from 2 up to $10^5$ $M_{\odot}$. The effects of the general relativity had been taken into account. The equation of state in the temperature and density ranges $10^9 < T < 10^{10} K$, $10^5 < ρ< 10^{10}\,\frac{g}{cm^3}$ had been taken from the work of Imshennik and Nadyozhin (1965). The critical parameters for the values of entropy and stellar masses differ from more accurate values, obtained using a more complicated variant of accepted density distribution, not more than 12$\%$. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2511_03419 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Stellar critical parameters in the uniform density approximation Bisnovatyi-Kogan, G. S. Patraman, E. A. High Energy Astrophysical Phenomena Stellar models are calculated in the approximation of a uniform density distribution. Variational method was used for determination of the boundary of a stability loss, for stellar masses in the range from 2 up to $10^5$ $M_{\odot}$. The effects of the general relativity had been taken into account. The equation of state in the temperature and density ranges $10^9 < T < 10^{10} K$, $10^5 < ρ< 10^{10}\,\frac{g}{cm^3}$ had been taken from the work of Imshennik and Nadyozhin (1965). The critical parameters for the values of entropy and stellar masses differ from more accurate values, obtained using a more complicated variant of accepted density distribution, not more than 12$\%$. |
| title | Stellar critical parameters in the uniform density approximation |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2511.03419 |