2014
DOI: 10.1103/physrevd.89.103509
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Maximal neutron star mass and the resolution of the hyperon puzzle in modified gravity

Abstract: The so-called "hyperonization puzzle" in the theory of neutron stars is considered in the framework of modified f (R) gravity. We show that for simple hyperon equations of state, it is possible to obtain the maximal neutron star mass which satisfies the recent observational data for PSR J1614-2230, in higher-derivative models with power-law terms as f (R) = R+γR 2 +βR 3 . The soft hyperon equation of state under consideration is usually treated as non-realistic in the standard General Relativity. The numerical… Show more

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Cited by 243 publications
(168 citation statements)
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References 99 publications
(114 reference statements)
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“…This model has quite appealing phenomenological features, since as was shown in Ref. [24], when this model is employed to neutron stars, it generates an increase in the maximal neutron star mass, which is a very interesting phenomenological feature. Our purpose is to find which mimetic scalar potential V (φ = t) and Lagrange multiplier generates a cosmological evolution compatible with observations, for the F (R) gravity of Eq.…”
Section: Concordance With Observations Using Lagrange-multiplier mentioning
confidence: 99%
“…This model has quite appealing phenomenological features, since as was shown in Ref. [24], when this model is employed to neutron stars, it generates an increase in the maximal neutron star mass, which is a very interesting phenomenological feature. Our purpose is to find which mimetic scalar potential V (φ = t) and Lagrange multiplier generates a cosmological evolution compatible with observations, for the F (R) gravity of Eq.…”
Section: Concordance With Observations Using Lagrange-multiplier mentioning
confidence: 99%
“…4), while for a neutron star, with increasing radius, the mass decreases, (see Ref. (Astashenok 2014) for more details). In other words, there are critical values for Λ and α, so that, the diagram related to gravitational mass versus radius is not similar to the diagram related to ordinary neutron star.…”
Section: Maximum Mass Of Neutron Starmentioning
confidence: 99%
“…What I and others guess is that, just as the 3-body force is repulsive, higher terms in the EFT-EOS must also make it stiffer, to later soften into something phenomenologically viable when other degrees of freedom activate. Of course, another logical possibility is to have doubly exotic physics: new gravity phenomena (such as f (R) corrections to the Einstein-Hilbert action) providing the margin for the EOS to actually be softer [54].…”
Section: Resultsmentioning
confidence: 99%