Rotating neutron stars with quark cores

Rather, Ishfaq A.; Rahaman, Usuf; Imran, Mohammad; Das, Harish Chandra; Usmani, A. A.; Patra, S. K.

doi:10.1103/physrevc.103.055814

Cited by 30 publications

(11 citation statements)

References 139 publications

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“…A major challenge for realistic but still standard neutron star EoS models is producing a large maximum mass. Reaching masses as high as that of the light component of the GW190814 event is very difficult, specially when including hyperonic degrees of freedom (without resorting to fast rotation [11,12,16,23,[129][130][131][132], or strong magnetic fields [133]). Reaching masses as high as the companion of V723 Mon would not be possible at all with most standard EoS models.…”

Section: B How To Construct the Heaviest Neutron Starsmentioning

confidence: 99%

Extreme matter meets extreme gravity: Ultraheavy neutron stars with phase transitions

et al. 2022

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The speed of sound of the matter within neutron stars may contain non-smooth structure related to first-or higher-order phase transitions. Here we investigate what are the observable consequences of structure in the speed of sound, such as bumps, spikes, step functions, plateaus, and kinks. One of the main consequences is the possibility of ultra-heavy neutron stars (with masses larger than 2.5 solar masses) and mass twins in heavy (with masses larger than 2 solar masses) and ultra-heavy neutron stars. These stars pass all observational and theoretical constraints, including those imposed by recent LIGO/Virgo gravitational-wave observations and NICER X-ray observations. We thoroughly investigate other consequences of this structure in the speed of sound to develop an understanding of how non-smooth features affect astrophysical observables, such as stellar radii, tidal deformability, moment of inertia, and Love number. Our results have important implications for future gravitational wave and X-ray observations of neutron stars and their impact in nuclear astrophysics.

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Section: B How To Construct the Heaviest Neutron Starsmentioning

confidence: 99%

Extreme matter meets extreme gravity: Ultraheavy neutron stars with phase transitions

et al. 2022

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“…A major challenge for realistic but still standard neutron star EoS models is producing a large maximum mass. Reaching masses as high as that of the light component of the GW190814 event is very difficult, specially when including hyperonic degrees of freedom (without resorting to fast rotation [11,12,16,23,[125][126][127][128], or strong magnetic fields [129]). Reaching masses as high as the companion of V723 Mon would not be possible at all with most standard EoS models.…”

Section: B How To Construct the Heaviest Neutron Starsmentioning

confidence: 99%

Extreme Matter meets Extreme Gravity: Ultra-heavy neutron stars with crossovers and first-order phase transitions

Tan,

Dore,

Dexheimer

et al. 2021

Preprint

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The speed of sound of the matter within neutron stars may contain non-smooth structure related to first-order phase transitions or crossovers. Here we investigate what are the observable consequences of structure in the speed of sound, such as bumps, spikes, step functions, plateaus, and kinks. One of the main consequences is the possibility of ultra-heavy neutron stars (with masses larger than 2.5 solar masses) and mass twins in heavy (with masses larger than 2 solar masses) and ultra-heavy neutron stars. These stars pass all observational and theoretical constraints, including those imposed by recent LIGO/Virgo gravitational-wave observations and NICER X-ray observations. We thoroughly investigate other consequences of this structure in the speed of sound to develop an understanding of how non-smooth features affect astrophysical observables, such as stellar radii, tidal deformability, moment of inertia, and Love number. Our results have important implications for future gravitational wave and X-ray observations of neutron stars and their impact in nuclear astrophysics.

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“…The concept of hybrid star is another vital inference from recent astrophysical observations and studied in various recent works (Nandi & Char 2018;Gomes et al 2019c;Paschalidis et al 2018;Mar-iani et al 2019;Nandi & Pal 2021;Rather et al 2021) as already mentioned in sec. 1.…”

Section: Discussionmentioning

confidence: 99%

Compact star merger events with stars composed of interacting strange quark matter

Kumar,

Thapa,

Sinha

2022

Preprint

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We investigate the properties of stars participating in double compact star merger events considering interacting model of stable strange quark matter. We model the matter making it compatible with the recent astrophysical observations of compact star mass-radius and gravitational wave events. In this context we consider modified MIT bag model and vector bag model with and without self interaction. We find new upper bound on tidal deformability of 1.4 𝑀 strange star corresponding to the upper bound of effective tidal deformability inferred from gravitational wave event. Range of compactness of 1.4 𝑀 strange star is obtained as 0.175 ≤ 𝐶 1.4 ≤ 0.199. Radius range of 1.5𝑀 primary star is deduced to be 10.57 ≤ 𝑅 1.5 ≤ 12.04 km, following stringent GW170817 constraints. GW190425 constraints provide with upper limit on radius of 1.7 solar mass strange star that it should be less than 13.41 km.

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Rotating neutron stars with quark cores

Cited by 30 publications

References 139 publications

Extreme matter meets extreme gravity: Ultraheavy neutron stars with phase transitions

Extreme matter meets extreme gravity: Ultraheavy neutron stars with phase transitions

Extreme Matter meets Extreme Gravity: Ultra-heavy neutron stars with crossovers and first-order phase transitions

Compact star merger events with stars composed of interacting strange quark matter

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