Affiliation:
1. Department of Physics, Indian Institute of Technology Kanpur , Kanpur 208016, India
Abstract
ABSTRACT
The Schönberg–Chandrasekhar limit in post-main-sequence evolution for stars of masses in the range 1.4 ≲ M/M⊙ ≲ 6 gives the maximum pressure that the stellar core can withstand, once the central hydrogen is exhausted. It is usually expressed as a quadratic function of 1/α, with α being the ratio of the mean molecular weight of the core to that of the envelope. Here, we revisit this limit in scenarios where the pressure balance equation in the stellar interior may be modified, and in the presence of small stellar pressure anisotropy, that might arise due to several physical phenomena. Using numerical analysis, we derive a three parameter-dependent master formula for the limit, and discuss various physical consequences. As a by-product, in a limiting case of our formula, we find that in the standard Newtonian framework, the Schönberg–Chandrasekhar limit is best-fit by a polynomial that is linear, rather than quadratic, to lowest order in 1/α.
Publisher
Oxford University Press (OUP)
Subject
Space and Planetary Science,Astronomy and Astrophysics
Cited by
2 articles.
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