Constraining gravity with hadron physics: neutron stars, modified gravity and gravitational waves

Llanes-Estrada, Felipe J.

doi:10.1051/epjconf/201713701013

Cited by 6 publications

(9 citation statements)

References 58 publications

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“…The answer seems positive as far as the simulations based work by Bauswein et al [130,131] on the merger process of two strange stars indicate. However, eventually, that depends on the puzzle of alternative gravity, i.e., the degeneracy in understanding both the equation of state and modified gravity (MG) [132]. On constraining recent gravitational wave observations of binary BH mergers, Motohashi and Minamitsuji [133] have classified GR solutions in MG based on their retrieval status from MG → GR.…”

Section: Discussionmentioning

confidence: 99%

Study on Anisotropic Strange Stars in f ( T , T ) Gravity

Salako

Khlopov

Ray³

et al. 2020

Universe

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In this work, we study the existence of strange stars in the background of f(T,T) gravity in the Einstein spacetime geometry, where T is the torsion tensor and T is the trace of the energy-momentum tensor. The equations of motion are derived for anisotropic pressure within the spherically symmetric strange star. We explore the physical features like energy conditions, mass-radius relations, modified Tolman–Oppenheimer–Volkoff (TOV) equations, principal of causality, adiabatic index, redshift and stability analysis of our model. These features are realistic and appealing to further investigation of properties of compact objects in f(T,T) gravity as well as their observational signatures.

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Section: Discussionmentioning

confidence: 99%

Study on Anisotropic Strange Stars in f ( T , T ) Gravity

Salako

Khlopov

Ray³

et al. 2020

Universe

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“…Before the detection of GW170817 it was considered possible that a double neutron-star merger would be found within the first three aLIGO runs [29]. At the time of Confinement XII [5], none had been detected to a distance of 70 Megaparsec (100 MPc in the case of merging NS-BH). Various studies were predicting between 0.2 and 200 NS-NS merger detections per year of aLIGO operation.…”

Section: How Many Events Should We Expect?mentioning

confidence: 99%

“…Circulating clockwise from the top-left corner of the figure we find [5] the following notes (in red online, those of special interest for hadron physics).…”

Section: Anatomy Of a Gw Signal In A Ns Binary Mergermentioning

confidence: 99%

“…In relation to tidal polarizability, the amount of ejecta determined from the EM observations implies a lower limit of Λ > 300 [195], but this limit was obtained considering only four EoS models.In general, radius and tidal polarizability are correlated and its is easy to convert this radius constraint to a limit on Λ = 2 3 k 2 ( c 2 R GM ) 5 . [185] shows that this radius constraint implies that Λ ≥ 180 (for n tr = 2n 0 and the CSM).…”

Section: Comparison Of MM and Csmmentioning

confidence: 99%

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Hadron matter in neutron stars in view of gravitational wave observations

Llanes-Estrada

Lope-Oter

2019

Progress in Particle and Nuclear Physics

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In this review we highlight a few physical properties of neutron stars and their theoretical treatment inasmuch as they can be useful for nuclear and particle physicists concerned with matter at finite density (and newly, temperature). Conversely, we lay out some of the hadron physics necessary to test General Relativity with binary mergers including at least one neutron star, in view of the event GW170817: neutron stars and their mergers reach the highest matter densities known, offering access to the matter side of Einstein's equations. In addition to minimum introductory material for those interested in starting research in the field of neutron stars, we dedicate quite some effort to a discussion of the Equation of State of hadron matter in view of gravitational wave developments; we address phase transitions and how the new data may help; we show why transport is expected to be dominated by turbulence instead of diffusion through most if not all of the star, in view of the transport coefficients that have been calculated from microscopic hadron physics; and we relate many of the interesting physics topics in neutron stars to the radius and tidal deformability.

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“…However, our point here [8] is that an EoS determined this way cannot be used to constrain theories beyond General Relativity because it already assumes GR (in its use of Tolman-Oppenheimer-Volkoff equations to calculate an observational mass-radius diagram, or in its use of the GR gravitational wave solutions, for example). To avoid circular reasoning, the community needs an effort to provide EoS purely from hadron theory.…”

Section: Introductionmentioning

confidence: 99%

nEoS: neutron star equation of state from hadron physics alone

Lope-Oter

Windisch

Llanes-Estrada

et al. 2019

J. Phys. G: Nucl. Part. Phys.

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We contribute a publicly available set of tables and code to provide Equations of State (EoS) for matter at neutron star densities. Our EoSes are constrained only by input from hadron physics and fundamental principles, without feedback from neutron star observations, and so without relying on General Relativity. They can therefore be used to test General Relativity itself, as well as modified gravity theories, with neutron star observables, without logical circularity. We have adapted state of the art results from N N chiral potentials for the low-density limit, pQCD results for the asymptotically high-density EoS, and use monotonicity and causality as the only restrictions for intermediate densities, for the EoS sets to remain as modelindependent as is feasible today.

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Constraining gravity with hadron physics: neutron stars, modified gravity and gravitational waves

Cited by 6 publications

References 58 publications

Study on Anisotropic Strange Stars in f ( T , T ) Gravity

Study on Anisotropic Strange Stars in f ( T , T ) Gravity

Hadron matter in neutron stars in view of gravitational wave observations

nEoS: neutron star equation of state from hadron physics alone

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