Critical mass, moment of inertia and universal relations of rapidly rotating neutron stars with exotic matter

Lenka, Smruti Smita; Char, Prasanta; Banik, Sarmistha

doi:10.1142/s0218271817501279

Cited by 16 publications

(11 citation statements)

References 49 publications

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“…This holds good for other observable quantities also. When the ratio of critical mass i.e., the maximum mass at the mass-shedding limit and maximum mass for static neutron stars are plotted with normalised angular momentum with respect to maximum angular momentum, it also shows a universal relation [39,40]. However, this universality appears to be lost when we look at both HQ EoSs.…”

Section: Resultsmentioning

confidence: 90%

Moment of inertia, quadrupole moment, Love number of neutron star and their relations with strange-matter equations of state

et al. 2018

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We investigate the impact of strange matter equations of state involving Λ hyperons, Bose-Einstein condensate of K − mesons and first order hadron-quark phase transition on moment of inertia, quadrupole moment and tidal deformability parameter of slowly rotating neutron stars. All these equations of state are compatible with the 2 M solar constraint. The main findings of this investigation are the universality of the I-Q and I-Love number relations, which are preserved by the EoSs including Λ hyperons and antikaon condensates, but broken in presence of a first order hadron-quark phase transition. Furthermore, it is also noted that the quadrupole moment approaches the Kerr value of a black hole for maximum mass neutron stars.PACS. 9 7.60.Jd neutron stars -26.60.Kp equations of state

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Section: Resultsmentioning

confidence: 90%

Moment of inertia, quadrupole moment, Love number of neutron star and their relations with strange-matter equations of state

et al. 2018

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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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“…Because we evaluate the stability of our neutron-star sequences in the absence of rotation, we are excluding supramassive (i.e. rotationstabilized) neutron stars, for which the universal relations deteriorate at high compactness[79].…”

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confidence: 99%

Inferring neutron star properties from GW170817 with universal relations

Kumar

Landry

2019

Phys. Rev. D

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Because all neutron stars share a common equation of state, tidal deformability constraints from the compact binary coalescence GW170817 have implications for the properties of neutron stars in other systems. Using equation-of-state insensitive relations between macroscopic observables like moment of inertia (I), tidal deformability (Λ) and stellar compactness, we derive constraints on these properties as a function of neutron-star mass based on the LIGO-Virgo collaboration's canonical deformability measurement, Λ1.4 = 190 +390 −120 . Specific estimates of Λ, I, dimensionless spin χ, and stellar radius R for a few systems targeted by radio or X-ray studies are extracted from the general constraints. We also infer the canonical neutron-star radius as R1.4 = 10.9 +1.9 −1.5 km at 90% confidence. We further demonstrate how a gravitational-wave measurement of Λ1.4 can be combined with independent measurements of neutron-star radii to tighten constraints on the tidal deformability as a proxy for the equation of state. We find that GW170817 and existing observations of six thermonuclear bursters in low-mass X-ray binaries jointly imply Λ1.4 = 196 +92 −63 at the 90% confidence level.1 A different universal relation has been used elsewhere in conjunction with GW170817 to constrain the maximum mass of nonrotating neutron stars [26]. 2 In the remainder of the paper, quoted error bars refer to symmetric 90% confidence intervals about the median unless otherwise specified. 3 Note added: A Bayesian analysis of this kind-but focused on the stellar radius, rather than the tidal deformability-is presented in Ref.[45], which appeared shortly after completion of this paper.

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Critical mass, moment of inertia and universal relations of rapidly rotating neutron stars with exotic matter

Cited by 16 publications

References 49 publications

Moment of inertia, quadrupole moment, Love number of neutron star and their relations with strange-matter equations of state

Moment of inertia, quadrupole moment, Love number of neutron star and their relations with strange-matter equations of state

Universal relations for rapidly rotating cold and hot hybrid star

Inferring neutron star properties from GW170817 with universal relations

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