Nonperturbative models of quark stars in $f$(R) gravity
By Artyom V. Astashenok, Salvatore Capozziello, Sergei D. Odintsov. 2014
140 citations recorded by the source corpus.
Abstract Quark star models with realistic equation of state in nonperturbative f ( R ) gravity are considered. The mass-radius relation for f ( R ) = R + α R 2 model is obtained. Considering scalar curvature R as an independent function, one can find out, for each value of central density, the unique value of central curvature for which one has solutions with the required asymptotic R → 0 for r → ∞ . In other words, one needs a fine-tuning for R to achieve quark stars in f ( R ) gravity. We consider also the analogue description in corresponding scalar-tensor gravity. The fine-tuning on R is equivalent to the fine-tuning on the scalar field ϕ in this description. For distant observers, the gravitational mass of the star increases with increasing α ( α > 0 ) but the interpretation of this fact depends on frame where we work. Considering directly f ( R ) gravity, one can say that increasing of mass occurs by the “gravitational sphere” outside the star with some “effective mass”. On the other hand, in conformal scalar-tensor theory, we also have a dilaton sphere (or “disphere”) outside the star but its contribution to gravitational mass for distant observer is negligible. We show that it is possible to discriminate modified theories of gravity from General Relativity due to the gravitational redshift of the thermal spectrum emerging from the surface of the star.
Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics, Oceanography
View Paper: https://www.semanticscholar.org/paper/8e89d744bc64dbedd009d7ec06b2ebf869131db7
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Citations in the corpus
- Stellar equilibrium configurations of compact stars in f(R,T) theory of gravity (2015, methodology): “Moreover, the TOV equations derived for different modified gravity models [8, 9, 34, 35] have contributed to the understanding of compact stars structure and matter at high densities.”