Hot Neutron Star Matter and Proto-neutron Stars

Farrell, Delaney; Alp, A; Spinella, William M.; Weber, Fridolin; Malfatti, Germán; Orsaria, M.; Ranea‐Sandoval, Ignacio F.

doi:10.1142/9789811220913_0005

Cited by 3 publications

(4 citation statements)

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“…In the results presented in this work, the temperature is held fixed and entropy calculated. The numerical procedure can be completed by instead holding entropy fixed; see Farrell et al (2023), for an example.…”

Section: Properties Of Nuclear Matter At Zero and Finite Temperaturementioning

confidence: 99%

Relativistic Brueckner–Hartree–Fock Calculations for Cold and Hot Neutron Stars

Farrell,

Weber

2024

ApJ

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This study investigates the properties of symmetric and asymmetric nuclear matter using the relativistic Brueckner–Hartree–Fock formalism, examining both zero and finite temperatures up to 70 MeV. Employing the full Dirac space, we incorporate three Bonn potentials (A, B, and C), which account for meson masses, coupling strengths, cutoff parameters, and form factors. The calculated properties of asymmetric nuclear matter form the basis for constructing equation-of-state (EOS) models tailored for neutron stars. These models, in turn, enable the computation of bulk properties for nonrotating, uniformly rotating, and differentially rotating neutron stars. Notably, the EOS models studied in this paper are sufficiently versatile to accommodate the mass of the most massive neutron star ever detected, PSR J0952–0607, estimated to be 2.35 ± 0.17 M ⊙. Furthermore, they yield masses and radii for PSR J0030+451 that align with the confidence intervals established for this pulsar.

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Section: Properties Of Nuclear Matter At Zero and Finite Temperaturementioning

confidence: 99%

Relativistic Brueckner–Hartree–Fock Calculations for Cold and Hot Neutron Stars

Farrell,

Weber

2024

ApJ

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“…The densities shown in Equations ( 25) and ( 32) are for compact star matter at zero temperature. In the case of the matter at finite temperature, these densities are given by [32] n s B = (2J B + 1)…”

Section: Dyson Equation and Baryon Self-energiesmentioning

confidence: 99%

“…Spacetime is flat on the length scale of particle interactions inside a neutron star (∼1 fm), so the flat space Minkowski metric can be used. This leads to the following expressions for the energy density ε = T 00 to [15,22,32,33]…”

Section: Equation Of State In Standard Rmf Theorymentioning

confidence: 99%

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Gravitational-Wave Instabilities in Rotating Compact Stars

et al. 2022

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It is generally accepted that the limit on the stable rotation of neutron stars is set by gravitational-radiation reaction (GRR) driven instabilities, which cause the stars to emit gravitational waves that carry angular momentum away from them. The instability modes are moderated by the shear viscosity and the bulk viscosity of neutron star matter. Among the GRR instabilities, the f-mode instability plays a historically predominant role. In this work, we determine the instability periods of this mode for three different relativistic models for the nuclear equation of state (EoS) named DD2, ACB4, and GM1L. The ACB4 model for the EoS accounts for a strong first-order phase transition that predicts a new branch of compact objects known as mass-twin stars. DD2 and GM1L are relativistic mean field (RMF) models that describe the meson-baryon coupling constants to be dependent on the local baryon number density. Our results show that the f-mode instability associated with m=2 sets the limit of stable rotation for cold neutron stars (T≲1010 K) with masses between 1M⊙ and 2M⊙. This mode is excited at rotation periods between 1 and 1.4 ms (∼20% to ∼40% higher than the Kepler periods of these stars). For cold hypothetical mass-twin compact stars with masses between 1.96M⊙ and 2.10M⊙, the m=2 instability sets in at rotational stellar periods between 0.8 and 1 millisecond (i.e., ∼25% to ∼30% above the Kepler period).

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Differential rotation in neutron stars at finite temperatures

Farrell,

Weber,

Negreiros

2024

Front. Phys.

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IntroductionThis paper investigates the impact of differential rotation on the bulk properties and onset of rotational instabilities in neutron stars at finite temperatures up to 50 MeV.MethodsUtilizing the relativistic Brueckner-Hartree-Fock (RBHF) formalism in full Dirac space, the study constructs equation of state (EOS) models for hot neutron star matter, including conditions relevant for high temperatures. These finite-temperature EOS models are applied to compute the bulk properties of differentially rotating neutron stars with varying structural deformations.ResultsThe findings demonstrate that the stability of these stars against bar-mode deformation, a key rotational instability, is only weakly dependent on temperature. Differential rotation significantly affects the maximum mass and radius of neutron stars, and the threshold for the onset of bar-mode instability shows minimal sensitivity to temperature changes within the examined range.DiscussionThese findings are crucial for interpreting observational data from neutron star mergers and other high-energy astrophysical events. The research underscores the necessity of incorporating differential rotation and finite temperature effects in neutron star models to predict their properties and stability accurately.

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Hot Neutron Star Matter and Proto-neutron Stars

Cited by 3 publications

References 100 publications

Relativistic Brueckner–Hartree–Fock Calculations for Cold and Hot Neutron Stars

Relativistic Brueckner–Hartree–Fock Calculations for Cold and Hot Neutron Stars

Gravitational-Wave Instabilities in Rotating Compact Stars

Differential rotation in neutron stars at finite temperatures

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