Slowly rotating neutron and strange stars in R 2 gravity
Kalin V. Staykov,Kalin V. Staykov,Daniela D. Doneva,Daniela D. Doneva,Stoytcho S. Yazadjiev,Stoytcho S. Yazadjiev,Kostas D. Kokkotas,Kostas D. Kokkotas +7 more
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In this article, the structure of the slowly rotating neutron stars in R-squared gravity with Lagrangian f(R) = R + aR2, where a is a parameter.Abstract:
In the present paper we investigate self-consistently slowly rotating neutron and strange stars in R-squared gravity with Lagrangian f(R) = R + aR2, where a is a parameter. For this purpose we first derive the equations describing the structure of the slowly rotating compact stars in f(R)-gravity and then simultaneously solve numerically the exterior and the interior problem. The structure of the slowly rotating neutron stars is studied for two different hadronic equations of state and a strange matter equation of state. The moment of inertia and its dependence on the stellar mass and the R-squared gravity parameter a is also examined in details. The numerical results show that the neutron star moment of inertia can be up to 30% larger compared to the corresponding general relativistic models. This is much higher than the change in the maximum mass induced by R-squared gravity and is beyond the EOS uncertainty. In this way the future observations of the moment of inertia of compact stars could allow us to distinguish between general relativity and f(R) gravity, and more generally to test the strong field regime of gravity.read more
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Modified gravity theories on a nutshell: Inflation, bounce and late-time evolution
TL;DR: In this paper, the authors systematically review some standard issues and also the latest developments of modified gravity in cosmology, emphasizing on inflation, bouncing cosmology and late-time acceleration era.
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Stellar equilibrium configurations of compact stars in $f(R,T)$ gravity
TL;DR: In this paper, the authors derived the hydrostatic equilibrium configuration of neutron stars and strange stars, whose fluid pressure is computed from the equations of state for the f(R,T) theory of gravity, with $R$ and $T$ standing for the Ricci scalar and trace of the energy-momentum tensor, respectively.
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Stellar equilibrium configurations of compact stars in f(R,T) theory of gravity
TL;DR: In this paper, the authors study the hydrostatic equilibrium configuration of neutron stars and strange stars, whose fluid pressure is computed from the equations of state p=ωρ5/3 and p=028(ρ−4ℬ), respectively, with ω and ℬ being constants and ρ the energy density of the fluid.
References
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TL;DR: In this article, the authors present a review of the most important aspects of the different classes of modified gravity theories, including higher-order curvature invariants and metric affine.
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Unified cosmic history in modified gravity: from F(R) theory to Lorentz non-invariant models
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A two-solar-mass neutron star measured using Shapiro delay
Paul Demorest,Timothy T. Pennucci,Scott M. Ransom,Mallory S. E. Roberts,Jason W. T. Hessels,Jason W. T. Hessels +5 more
TL;DR: Radio timing observations of the binary millisecond pulsar J1614-2230 that show a strong Shapiro delay signature are presented and the pulsar mass is calculated to be (1.97 ± 0.04)M⊙, which rules out almost all currently proposed hyperon or boson condensate equations of state.
Journal ArticleDOI
A massive pulsar in a compact relativistic binary
John Antoniadis,Paulo C. C. Freire,Norbert Wex,Thomas M. Tauris,Ryan S. Lynch,Marten H. van Kerkwijk,Michael Kramer,Michael Kramer,C. G. Bassa,V. S. Dhillon,T. Driebe,Jason W. T. Hessels,Jason W. T. Hessels,Victoria M. Kaspi,V. I. Kondratiev,V. I. Kondratiev,Norbert Langer,Tom Marsh,Maura McLaughlin,Timothy T. Pennucci,Scott M. Ransom,Ingrid H. Stairs,Joeri van Leeuwen,Joeri van Leeuwen,Joris P. W. Verbiest,David G. Whelan +25 more
TL;DR: Pulsar J0348+0432 is only the second neutron star with a precisely determined mass of 2 M☉
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