Dilatonic equation of hydrostatic equilibrium and neutron star structure

Hendi, S. H.; Bordbar, G. H.; Panah, B. Eslam; Najafi, Mohammad Bagher

doi:10.1007/s10509-015-2429-x

Cited by 30 publications

(30 citation statements)

References 79 publications

(67 reference statements)

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“…It was shown that the maximum mass of neutron star is about 1.68M ⊙ . In addition, the EoS with dilaton gravity was employed and the properties of neutron star were investigated [56]. The results showed that by increasing the effects of dilaton gravity, the maximum mass of this star decreases (M max ≤ 1.68M ⊙ ).…”

Section: B Mass-radius Relation and Other Properties Of Neutron Starmentioning

confidence: 99%

Neutron stars structure in the context of massive gravity

Hendi

Bordbar

Panah

et al. 2017

J. Cosmol. Astropart. Phys.

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Motivated by the recent interests in spin−2 massive gravitons, we study the structure of neutron star in the context of massive gravity. The modifications of TOV equation in the presence of massive gravity are explored in 4 and higher dimensions. Next, by considering the modern equation of state for the neutron star matter (which is extracted by the lowest order constrained variational (LOCV) method with the AV18 potential), different physical properties of the neutron star (such as Le Chatelier's principle, stability and energy conditions) are investigated. It is shown that consideration of the massive gravity has specific contributions into the structure of neutron star and introduces new prescriptions for the massive astrophysical objects. The mass-radius relation is examined and the effects of massive gravity on the Schwarzschild radius, average density, compactness, gravitational redshift and dynamical stability are studied. Finally, a relation between mass and radius of neutron star versus the Planck mass is extracted.

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Section: B Mass-radius Relation and Other Properties Of Neutron Starmentioning

confidence: 99%

Neutron stars structure in the context of massive gravity

Hendi

Bordbar

Panah

et al. 2017

J. Cosmol. Astropart. Phys.

View full text Add to dashboard Cite

show abstract

“…Finally, substituting eq. (36) back into (35) and into (34), we will get equation of states with fixed temperature and electric charges…”

Section: Thermodynamic Definitions In the Extended Phase Spacementioning

confidence: 99%

“…We will try to understand this question from both thermo-ensemble and dynamical perturbation analysis. While previous works [19,20,[33][34][35][36][37][38][39] are mainly from thermo-ensemble aspects. Our dynamic consideration borrow ideas from ref.…”

Section: Introductionmentioning

confidence: 99%

Phase structure and quasinormal modes of a charged AdS dilaton black hole

Shi

Zeng

2018

Phys. Rev. D

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We investigate the phase structure of a charged AdS dilaton black hole in the extended phase space which takes the cosmological constant, i.e. the AdS-Λ parameter as pressures. Through both thermal ensemble and quasinormal mode analysis, we find that stable phase of the black hole with non-trivial dilaton profiles always exists for both large and small couplings when the AdS-Λ is considered dynamical degrees of freedom. This forms a somewhat contrast with previous works which does not do so. Our results provide new examples for the parallelism or equivalences between thermal ensemble methods and dynamic perturbation analysis for black hole phase structures.

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“…Thanks to the discovery of a neutron star with mass 1.974M [49]-confirmed later on by other measurements [50][51][52][53], the precise sighting [54] through binary system measurements, double neutron stars features and pulsar systems [55], the validity of GR standard predictions have been indeed put into question. Thus the interest for such configurations in extended theories of gravity, mainly in scalar-tensor theories [56][57][58][59][60][61][62][63][64][65][66][67][68][69][70][71], has aimed to reconcile predictions with astrophysical results.…”

Section: Spherical Configurations: Neutron Starsmentioning

confidence: 99%

Towards New Constraints in Extended Theories of Gravity: Cosmography and Gravitational-Wave Signals from Neutron Stars

Cruz-Dombriz

2018

Galaxies

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Combined cosmological, astrophysical and numerical tests may shed some light on the viability of theories of gravity beyond Einsteinian relativity. In this letter, we present two different techniques providing complementary ways of testing new physics beyond the ΛCDM cosmological paradigm. First, we shall present some of the latest progress and shortcomings in the cosmographic model-independent approach for several modified gravity theories using supernovae catalogues, baryonic acoustic oscillation data and H(z) differential age compilations. Second, we shall show how once the Einsteinian paradigm is abandoned, the phenomenology of neutron stars changes dramatically since neutron-star masses can be much larger than their General Relativity counterparts. Consequently, the total energy available for radiating gravitational waves could be of the order of several solar masses, and thus a merger of these stars constitutes a privileged wave source. Unfortunately at the present time our persisting lack of understanding in the strong interaction sector does not allow to distinguish the alternative theories from the usual General Relativity predictions.

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Dilatonic equation of hydrostatic equilibrium and neutron star structure

Cited by 30 publications

References 79 publications

Neutron stars structure in the context of massive gravity

Neutron stars structure in the context of massive gravity

Phase structure and quasinormal modes of a charged AdS dilaton black hole

Towards New Constraints in Extended Theories of Gravity: Cosmography and Gravitational-Wave Signals from Neutron Stars

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