Influence of the crust on the neutron star macrophysical quantities and universal relations

Suleiman, Lami; Fortin, M.; Zdunik, J. L.; Haensel, P.

doi:10.1103/physrevc.104.015801

Cited by 26 publications

(13 citation statements)

References 38 publications

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“…Thus, it is reasonable to expect that the perfect-fluid idealization will eventually break down, at least to some extent, and that solid phases of matter may be relevant for astronomical compact objects. This is indeed the situation in the crust of a neutron star [1,2], whose fundamental constituents are largely unknown, especially in the core [3].…”

Section: Introductionmentioning

confidence: 94%

“…A natural generalization of fluid models is to consider elastic materials [4][5][6][7][8], also studied perturbatively, to model the crust of a neutron star [1,2]. In this paper, we introduce a new systematic approach to the problem of self-gravitating elastic materials in general relativity (GR), which allows building elastic compact objects in a simple-yet general-way and assessing their viability in the strong-gravity regime.…”

Section: Introductionmentioning

confidence: 99%

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Compact elastic objects in general relativity

et al. 2022

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We introduce a rigorous and general framework to study systematically self-gravitating elastic materials within general relativity, and apply it to investigate the existence and viability, including radial stability, of spherically symmetric elastic stars. We present the mass-radius (M − R) diagram for various families of models, showing that elasticity contributes to increasing the maximum mass and the compactness up to ≈22%, thus supporting compact stars with mass well above two solar masses. Some of these elastic stars can reach compactness as high as GM=ðc 2 RÞ ≈ 0.35 while remaining stable under radial perturbations and satisfying all energy conditions and subluminal wave propagation, thus being physically realizable models of stars with a light ring. We provide numerical evidence that radial instability occurs for central densities larger than that corresponding to the maximum mass, as in the perfect-fluid case. Elasticity may be a key ingredient to building consistent models of exotic ultracompact objects and black hole mimickers, and can also be relevant for a more accurate modeling of the interior of neutron stars.

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Section: Introductionmentioning

confidence: 94%

Section: Introductionmentioning

confidence: 99%

Compact elastic objects in general relativity

et al. 2022

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“…At the same time, certain relations among global parameters of compact stars were established (Haensel & Zdunik 1989;Friedman et al 1989;Shapiro et al 1989;Haensel et al 1995;Lasota et al 1996;Haensel et al 2009) and intensively studied in recent years which are highly insensitive to the input EoS and, therefore, are named universal (Yagi & Yunes 2017). The universal relations have been derived for a variety of systems under different conditions, for example, both for non-rotating (Yagi & Yunes 2013;Sotani et al 2013;Majumder et al 2015;Steiner et al 2016;Lenka et al 2017;Wei et al 2019;Kumar & Landry 2019;Raduta et al 2020;Suleiman et al 2021), slowly-rotating (Silva et al 2016) and rapidly rotating stars (Breu & Rezzolla 2016;Paschalidis et al 2018;Riahi et al 2019;Bozzola et al 2019;Khadkikar et al 2021;Koliogiannis & Moustakidis 2020), magnetized stars (Haskell et al 2014), finite temperature stars (Raduta et al 2020;Khadkikar et al 2021) in alternative theories of gravity (Doneva et al 2014;Pappas et al 2019;Popchev et al 2019;Yagi & Stepniczka 2021) ★ E-mail: noshad.khosravilargani@uwr.edu.pl † E-mail: tobias.fischer@uwr.edu.pl and in binaries (Manoharan et al 2021). For a review see Yagi & Yunes (2017).…”

Section: Introductionmentioning

confidence: 99%

Universal relations for rapidly rotating cold and hot hybrid star

Largani,

Fischer,

Sedrakian

et al. 2021

Preprint

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Several global parameters of compact stars are related via empirical relations, which are (nearly) independent of the underlying equation of state of dense matter and, therefore, are said to be universal. We investigate the universality of relations that express the maximum mass and the radius of non-rotating and maximally rapidly rotating configurations, as well as their moment of inertia, in terms of the compactness of the star. For this, we first utilize a collection of cold (zero-temperature) and hot (isentropic) nucleonic EoS and confirm that the universal relations are holding for our collection of EoS. We then go on, to add to our collection and test for the same universality models of EoS which admit a strong first-order phase transition from nucleonic to deconfined quark matter. Also in this case we find that the universal relations hold, in particular for hot, isentropic hybrid stars. By fitting the universal relations to our computed data, we determine the coefficients entering these relations and the accuracy to which they hold.

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“…See also Ref. [12] for a recent study on the impact of non consistent treatment of crust and core EoS on NS macroscopic properties. Presently, the experimental uncertainties in the measurement of NS radii are still larger -about 1-2 km -than this theoretical one.…”

Section: Introductionmentioning

confidence: 99%

Confronting a set of Skyrme and $χ_{EFT}$ predictions for the crust of neutron stars

Grams,

Margueron,

Somasundaram

et al. 2022

Preprint

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With the improved accuracy of neutron star observational data, it is necessary to derive new equation of state where the crust and the core are consistently calculated within a unified approach. For this purpose we describe non-uniform matter in the crust of neutron stars employing a compressible liquid-drop model, where the bulk and the neutron fluid terms are given from the same model as the one describing uniform matter present in the core. We then generate a set of fifteen unified equations of state for cold catalyzed neutron stars built on realistic modelings of the nuclear interaction, which belongs to two main groups: the first one derives from the phenomenological Skyrme interaction and the second one from χEFT Hamiltonians. The confrontation of these model predictions allows us to investigate the model dependence for the crust properties, and in particular the effect of neutron matter at low density. The new set of unified equations of state is available at the CompOSE repository. Keywords neutron star • equation of state • crust • compressible liquid-drop model • Skyrme and chiral EFT interactions

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Influence of the crust on the neutron star macrophysical quantities and universal relations

Cited by 26 publications

References 38 publications

Compact elastic objects in general relativity

Compact elastic objects in general relativity

Universal relations for rapidly rotating cold and hot hybrid star

Confronting a set of Skyrme and $χ_{EFT}$ predictions for the crust of neutron stars

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