Equilibrium and stability of relativistic stars in extended theories of gravity

Wojnar, Aneta; Velten, Hermano

doi:10.1140/epjc/s10052-016-4549-z

Cited by 40 publications

(33 citation statements)

References 41 publications

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“…(please see Refs. [1][2][3][4][5][6][7][8][9] and the references therein for reviews). The discussions of the relation of the instability of anisotropic stars with perfect fluid energy condition have been reported in Refs.…”

Section: Introductionmentioning

confidence: 99%

Anisotropic neutron stars and perfect fluid’s energy conditions

Setiawan

Sulaksono

2019

Eur. Phys. J. C

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It is reported (Estevez-Delgado and Estevez-Delgado in Eur Phys J C 78:673, 2018) recently, that the absence of anisotropic in compact object pressure leads to a solution which is not physically acceptable due to the energy density and speed of sound can not be positive at the origin at the same time. Here, we calculate the pressure and energy density of NSs using realistic EOS predicted by a relativistic mean-field model including hyperons for isotropic and three different anisotropic pressure models such as the one of Doneva and Yazadjiev (

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Section: Introductionmentioning

confidence: 99%

Anisotropic neutron stars and perfect fluid’s energy conditions

Setiawan

Sulaksono

2019

Eur. Phys. J. C

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“…Let us consider the stability of stellar models (see Sec.1.2) for the simple scalar-tensor theories (19) with A = 1 and an arbitrary potential, i.e., [266]…”

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confidence: 99%

Stellar structure models in modified theories of gravity: Lessons and challenges

2020

Self Cite

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The understanding of stellar structure represents the crossroads of our theories of the nuclear force and the gravitational interaction under the most extreme conditions observably accessible. It provides a powerful probe of General Relativity on its strong field regime, and opens fruitful avenues for the exploration of new gravitational physics. The latter can be captured via the so-called modified theories of gravity, which modify the Einstein-Hilbert action of General Relativity and/or some of its building blocks/principles. These theories typically change the Tolman-Oppenheimer-Volkoff equations of stellar's hydrostatic equilibrium, having a large impact on the astrophysical properties of the corresponding stars, and thus opening a new window to constrain these theories with present and future observations of different types of stars. For relativistic stars, such as neutron stars, the uncertainty on the equation of state of matter at supranuclear densities intertwines with the new parameters coming from the modified gravity side, providing a whole new phenomenology for the typical predictions of stellar structure models, such as mass-radius relations, maximum masses, or moment of inertia. For non-relativistic stars, such as white, brown and red dwarfs, the weakening/strengthening of the gravitational force inside astrophysical bodies via the modified Newtonian (Poisson) equation may induce changes on the star's mass, radius, central density or luminosity, having an impact, for instance, in the Chandrasekhar's limit for white dwarfs, or in the minimum mass for stable hydrogen burning for high-mass brown dwarfs. This work aims to provide a broad overview of the main such results achieved in the recent literature for many such modified theories of gravity, by combining the results and constraints obtained from the analysis of relativistic and non-relativistic stars in different scenarios. Moreover, we will build a bridge between the efforts of the community working on different theories, formulations, types of stars, theoretical modellings, and observational aspects, highlighting some of the most promising opportunities in the field.

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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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Equilibrium and stability of relativistic stars in extended theories of gravity

Cited by 40 publications

References 41 publications

Anisotropic neutron stars and perfect fluid’s energy conditions

Anisotropic neutron stars and perfect fluid’s energy conditions

Stellar structure models in modified theories of gravity: Lessons and challenges

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

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