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Implications of q-deformed statistics on stellar stability

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  • Senay, M.

Abstract

Examination of Chandrasekhar’s equilibrium and stability condition for stars in the context of q-deformed Maxwell–Boltzmann statistics leads to the derivation of a new analytical formula that extends its classical case. This derivation assumes that the kinetic description of stellar matter conforms to a generalized Maxwell–Boltzmann distribution. It has been found that the maximum allowable radiation pressure at the center of a star for a given mass depends on the deformation parameter q. The classical Chandrasekhar condition is recovered in this framework when q equals 1.

Suggested Citation

  • Senay, M., 2024. "Implications of q-deformed statistics on stellar stability," Physica A: Statistical Mechanics and its Applications, Elsevier, vol. 656(C).
    • Handle: RePEc:eee:phsmap:v:656:y:2024:i:c:s0378437124006721
    DOI: 10.1016/j.physa.2024.130163
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    References listed on IDEAS

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    1. Kaniadakis, G. & Lissia, M. & Scarfone, A.M., 2004. "Deformed logarithms and entropies," Physica A: Statistical Mechanics and its Applications, Elsevier, vol. 340(1), pages 41-49.
    2. Tsallis, Constantino & Mendes, RenioS. & Plastino, A.R., 1998. "The role of constraints within generalized nonextensive statistics," Physica A: Statistical Mechanics and its Applications, Elsevier, vol. 261(3), pages 534-554.
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