Differentiating between sharp and smoother phase transitions in neutron stars

Pereira, Jonas P.; Bejger, Michał; Zdunik, J. Leszek; Haensel, Paweł

doi:10.48550/arxiv.2201.01217

Cited by 3 publications

(3 citation statements)

References 76 publications

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“…In this sense, more advanced detection techniques in the future, rendering more precise measurements for masses and radii of compact stars, hold promise for constraining their composition (see recent discussions in e.g., Refs. [72][73][74].…”

Section: B Stability Of Self-bound Quark Matter and The Equation Of S...mentioning

confidence: 99%

Interacting $ud$ and $uds$ quark matter at finite densities and quark stars

Yuan,

Li,

Miao

et al. 2022

Preprint

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The stability and equation of state of quark matter are studied within both two-flavor and (2+1)-flavor Nambu-Jona-Lasinio (NJL) models including the vector interactions. With a free parameter α, the Lagrangian is constructed by two parts, the original NJL Lagrangian and the Fierz transformation of it, as L = (1 − α)LNJL + αLFierz. We find that there is a possibility for both ud nonstrange and uds strange matter being absolute stable, depending on the interplay of the confinement with quark vector interaction and the exchange interaction channels. The calculated quark star properties can reconcile with the recently measured masses and radii of PSR J0030+0451 and PSR J0740+6620, as well as the tidal deformability of GW170817. Furthermore, the more strongly-interacting quark matter in the nonstrange stars allows a stiffer equation of state and consequently a higher maximum mass (∼ 2.7 M ) than the strange ones (∼ 2.1 M ). The sound velocities in strange and nonstrange quark star matter are briefly discussed compared to those of neutron star matter.

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Section: B Stability Of Self-bound Quark Matter and The Equation Of S...mentioning

confidence: 99%

Interacting $ud$ and $uds$ quark matter at finite densities and quark stars

Yuan,

Li,

Miao

et al. 2022

Preprint

View full text Add to dashboard Cite

show abstract

“…"Stability" means here the damping of radial disturbances, at least. Since the radii of configurations of the second (neutron stars) and third (hypothetical quark/hybrid stars [33][34][35][36][37][38][39][40]) islands are very similar, the notion of twin stars [31-33, 41, 42] has been coined for equal-mass configurations; "masquerade" was another related term [43].…”

Section: Introductionmentioning

confidence: 99%

Masses of compact (neutron) stars with distinguished cores

Zollner¹,

Ding²,

Kämpfer³

2023

Preprint

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The impact of the core mass on the compact/neutron-star mass-radius relation is studied. Besides the mass, the core is parameterized by its radius and surface pressure, which supports the outside one-component Standard Model (SM) matter. The core may accommodate SM matter with unspecified (or poorly known) equation-of-state or several components, e.g. consisting of admixtures of Dark Matter and/or Mirror World matter etc. beyond the SM. Thus, the admissible range of masses and radii of compact stars can be considerably extended.

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“…"Stability" means here the damping of radial disturbances. Since the radii of configurations of the second (neutron stars) and third (hypothetical quark/hybrid stars [25][26][27]) islands are very similar, the notion of twin stars [28,29] has been coined for equal-mass configurations; "masquerade" was another related term [30].…”

Section: Introductionmentioning

confidence: 99%

Exotic Cores with and without Dark-Matter Admixtures in Compact Stars

Zöllner¹,

Kämpfer²

2022

Preprint

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We parameterize the core of compact spherical star configurations by a mass (m x ) and a radius (r x ) and study the resulting admissible areas in the total-mass -total-radius plane. The employed fiducial equation-of-state models of the corona at radii r ≥ r x and pressures p ≤ p x = p(r = r x ) are that (i) of constant sound velocity and (ii) a proxy of DY∆ DD-ME2 provided by Buchdahl's exactly solvable ansatz. The core (r < r x ) may contain any type of material, e.g. Standard-Model matter with unspecified equation of state or/and an unspecified Dark-Matter admixture.Employing a toy model for the cool equation of state with first-order phase transition we discuss also the mass-radius relation of compact stars with an admixture of Dark Matter in a Mirror-World scenario.

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Differentiating between sharp and smoother phase transitions in neutron stars

Cited by 3 publications

References 76 publications

Interacting $ud$ and $uds$ quark matter at finite densities and quark stars

Interacting $ud$ and $uds$ quark matter at finite densities and quark stars

Masses of compact (neutron) stars with distinguished cores

Exotic Cores with and without Dark-Matter Admixtures in Compact Stars

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