White dwarfs in an ungravity-inspired model

Abstract

An ungravity-inspired model is employed to examine the astrophysical parameters of white dwarf stars (WDs) using polytropic and degenerate gas approaches. Based on the observed properties such as mass, radius, and luminosity of selected WDs, namely, Sirius B and $\epsilon$ Reticulum, bounds on the characteristic length and scaling dimension of the ungravity (UG) model are estimated. The UG effect on the Chandrasekhar limit for WDs is shown. The UG model is examined in the study of ultra-massive WDs, e.g., EUVE J1746-706. In the contact of UG inspired model, a new location for some WDs on the Hertzsprung-Russell diagram is found.

arXiv comment18 pages, 4 tables, 5 figures. Version to match the published one at Physical Review D93 (2016) no.10, 104046

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Cited by in corpus (10)

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• Significantly super-Chandrasekhar mass-limit of white dwarfs in noncommutative geometry
• Weak-field limit of $f(R)$ gravity to unify peculiar white dwarfs
• Cooling Process of White Dwarf Stars in Palatini $f(R)$ Gravity
• Modified virial theorem for highly magnetized white dwarfs
• Formation, Possible Detection and Consequences of Highly Magnetized Compact Stars
• On the impact of non-local gravity on compact stars
• Neutron Stars, Ungravity, and the I-Love-Q relation