Neutron stars in the braneworld within the Eddington-inspired Born-Infeld gravity

Prasetyo, Ilham; Husin, I.; Qauli, Ali Ikhsanul; Ramadhan, H. S.; Sulaksono, A.

doi:10.1088/1475-7516/2018/01/027

Cited by 19 publications

(11 citation statements)

References 84 publications

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“…The model was also studied in the context of higher-dimensional braneworlds by Prasetyo et al [475], assuming that the matter fields live on the brane while the bulk is empty. Using the Einstein-frame representation of the field equations, they use EOS which include hyperons under the form of the BSR23 parameter set of the ERMF model, and playing with the two parameters of the theory, ǫ and λ (the latter associated to the brane tension), they find neutron stars compatible with observational constraints (that is, M ∼ 2.1M ⊙ , r S ∼ 10km) for the (cosmologically and astrophysically acceptable) range 0 < ǫ < 6 × 10 6 m 2 , λ >> 1 MeV 4 .…”

Section: Eibi Gravitymentioning

confidence: 99%

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

2020

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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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Section: Eibi Gravitymentioning

confidence: 99%

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

2020

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“…A recently proposed way to alleviate the hyperon puzzle is to modify gravity at strong gravity field [22]. Consideration of compact stars in braneworld scenarios, leading to Einstein's equations reminiscent of EMSG for α > 0, is not new [23], and very recently, it was claimed that hyperon puzzle can be addressed, on account of nonlinear contributions of matter stress to the right-hand side of the Einstein's equations, in the Randall-Sundrum type-II braneworld in [24] and in the braneworld within the Eddington-inspired Born-Infeld gravity in [25]. In EMSG, the effective stiffening in the right-hand side of the Einstein equations, due to the new contributions of matter stresses under some conditions, may compensate the softening of the matter EoS due to the hyperonization and so enhance the maximum masses of NSs with hyperons.…”

Section: Introductionmentioning

confidence: 99%

Constraint on energy-momentum squared gravity from neutron stars and its cosmological implications

et al. 2018

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Deviations from the predictions of general relativity due to energy-momentum squared gravity (EMSG) are expected to become pronounced in the high density cores of neutron stars. We derive the hydrostatic equilibrium equations in EMSG and solve them numerically to obtain the neutron star mass-radius relations for four different realistic equations of state. We use the existing observational measurements of the masses and radii of neutron stars to constrain the free parameter, α, that characterizes the coupling between matter and spacetime in EMSG. We show that −10 −38 cm 3 /erg < α < +10 −37 cm 3 /erg. Under this constraint, we discuss what contributions EMSG can provide to the physics of neutron stars, in particular, their relevance to the so called hyperon puzzle in neutron stars. We also discuss how EMSG alters the dynamics of the early universe from the predictions of the standard cosmological model. We show that EMSG leaves the standard cosmology safely unaltered back to t ∼ 10 −4 seconds at which the energy density of the universe is ∼ 10 34 erg cm −3 .

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“…The theory is equivalent to Einstein's GR in vacuum but differs from it within matter. Since its introduction, various aspects of EiBI gravity have been studied by many researchers in the recent past, including black holes [47,[51][52][53][54][55][56][57][58][59][60], wormholes [61][62][63][64], compact stars [65][66][67][68][69], cosmological aspects [47,[70][71][72][73][74][75][76][77][78][79][80], astrophysical aspects [81][82][83], gravitational collapse [84,85], gravitational waves [86,87], implications in nongravitational contexts like particle physics [88] etc. See [89] for a recent review on various studies in EiBI gravity.…”

Section: Introductionmentioning

confidence: 99%

Wormholes with nonexotic matter in Born-Infeld gravity

Shaikh

2018

Phys. Rev. D

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We show that, in contrast to general relativity, in Eddington-inspired Born-Infeld gravity (EiBI), a violation of the null convergence condition does not necessarily lead to a violation of the null energy condition, by establishing a relationship between them. This serves as a motivation for finding wormhole solutions which can be supported by nonexotic matter in this gravity theory. We then obtain exact solutions of the field equations in EiBI gravity coupled to arbitrary nonlinear electrodynamics and anisotropic fluids. Depending on the signs and values of different parameters, the general solutions can represent both black holes and wormholes. In this work, we analyze the wormhole solutions. These wormholes are supported by nonexotic matter, i.e., matter satisfying all the energy conditions. As special cases of our general solutions, we work out several specific examples by considering Maxwell, power-law, Born-Infeld electrodynamics models and a particular form of an anisotropic fluid. * rajibul.shaikh@tifr.res.in

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Neutron stars in the braneworld within the Eddington-inspired Born-Infeld gravity

Cited by 19 publications

References 84 publications

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

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

Constraint on energy-momentum squared gravity from neutron stars and its cosmological implications

Wormholes with nonexotic matter in Born-Infeld gravity

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