Unified treatment of subsaturation stellar matter at zero and finite temperature

Gulminelli, F.; Raduta, Ad. R.

doi:10.1103/physrevc.92.055803

Cited by 133 publications

(115 citation statements)

References 106 publications

(289 reference statements)

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“…Once the EoS model is defined, the equilibrium configuration of inhomogeneous dense matter in the inner crust in full thermodynamic equilibrium at temperature T and baryon density n B is obtained following Lattimer & Swesty (1991); Gulminelli & Raduta (2015), who extended to finite temperature the variational formalism of Baym et al (1971a); Douchin and Haensel (2001).…”

Section: Model Of the Inner Crustmentioning

confidence: 99%

Crystallization of the inner crust of a neutron star and the influence of shell effects

Carreau

Gulminelli

Chamel

et al. 2020

A&A

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Context. In the cooling process of a non-accreting neutron star, the composition and properties of the crust are thought to be fixed at the finite temperature where nuclear reactions fall out of equilibrium. A lower estimation for this temperature is given by the crystallization temperature, which can be as high as ≈ 7 × 10 9 K in the inner crust, potentially leading to sizeable differences with respect to the simplifying cold-catalyzed matter hypothesis. Aims. We extend the recent work by Fantina et al. (2019) on the outer crust, to the study of the crystallization of the inner crust and the associated composition in the one-component plasma approximation.Methods. The finite temperature variational equations for non-uniform matter in both the liquid and the solid phases are solved using a compressible liquid-drop approach with parameters optimized on four different microscopic models which cover the present uncertainties in nuclear modeling. Results. We consider separately the effect of the different nuclear ingredients with their associated uncertainties, namely the nuclear equation of state, the surface properties in the presence of a uniform gas of dripped neutrons, and the proton shell effects arising from the ion single-particle structure. Our results suggest that the highest source of model dependence comes from the smooth part of the nuclear functional. Conclusions. We show that shell effects play an important role at the lowest densities close to the outer crust, but the most important physical ingredient to be settled for a quantitative prediction of the inner crust properties is the surface tension at extreme isospin values.

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Section: Model Of the Inner Crustmentioning

confidence: 99%

Crystallization of the inner crust of a neutron star and the influence of shell effects

Carreau

Gulminelli

Chamel

et al. 2020

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“…In this paper, we study the composition and formation of the outer crust of a non-accreting unmagnetized NS. After determining the crystallization temperature in the one-component plasma (OCP) approximation, the nuclear distributions and the impurity parameter are calculated fully self-consistently, adapting a general formalism originally developed for the description of a hot dense MCP under conditions prevailing in supernova cores (Gulminelli & Raduta 2015;Grams et al 2018). Our treatment of a OCP and a MCP plasma are presented in Sections 2 and 3, respectively.…”

Section: Introductionmentioning

confidence: 99%

Crystallization of the outer crust of a non-accreting neutron star

Fantina

Ridder

Chamel

et al. 2020

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Context. The interior of a neutron star is usually assumed to be made of cold catalyzed matter. However, the outer layers are unlikely to remain in full thermodynamic equilibrium during the formation of the star and its subsequent cooling, especially after crystallization occurs. Aims. We study the cooling and the equilibrium composition of the outer layers of a non-accreting neutron star down to crystallization. Here the impurity parameter, generally taken as a free parameter in cooling simulations, is calculated self-consistently using a microscopic nuclear model for which a unified equation of state has recently been determined. Methods. We follow the evolution of the nuclear distributions of the multi-component Coulomb liquid plasma fully self-consistently, adapting a general formalism originally developed for the description of supernova cores. We calculate the impurity parameter at the crystallization temperature as determined in the one-component plasma approximation.Results. Our analysis shows that the sharp changes in composition obtained in the one-component plasma approximation are smoothed out when a full nuclear distribution is allowed. The Coulomb coupling parameter at melting is found to be reasonably close to the canonical value of 175, except for specific values of the pressure for which supercooling occurs in the one-component plasma approximation. Our multi-component treatment leads to non-monotonic variations of the impurity parameter with pressure. Its values can change by several orders of magnitude reaching about 50, suggesting that the crust may be composed of an alternation of pure (highly conductive) and impure (highly resistive) layers. The results presented here complement the recent unified equation of state obtained within the same nuclear model. Conclusions. Our self-consistent approach to hot dense multi-component plasma shows that the presence of impurities in the outer crust of a neutron star is non-negligible and may have a sizeable impact on transport properties. In turn, this may have important implications not only for the cooling of neutron stars, but also for their magneto-rotational evolution.

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“…This approach is generally called "nuclear statistical equilibrium" (NSE). In the last years several models have been developed to go beyond a pure NSE and take into account nucleon interactions and the interaction of clusters with the surrounding medium at higher densities (see, e.g., [27,28,31,[61][62][63][64]). In stellar matter particular attention has to be paid to the interplay between the short-range nuclear interaction and the long-range Coulomb interaction, which determines sizes and shapes of the nuclear clusters and influences thus strongly the transition to homogeneous matter [65,66].…”

Section: A Statistical Model For Inhomogeneous Mattermentioning

confidence: 99%

New temperature dependent hyperonic equation of state: Application to rotating neutron star models and I−Q relations

et al. 2017

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In this work we present a newly constructed equation of state (EoS), applicable to stellar core collapse and neutron star mergers including the entire baryon octet. Our EoS is compatible with the main constraints from nuclear physics and, in particular, with a maximum mass for cold β-equilibrated neutron stars of 2M in agreement with recent observations. As an application of our new EoS, we compute numerical stationary models for rapidly (rigidly) rotating hot neutron stars. We consider maximum masses of hot stars, such as protoneutron stars or hypermassive neutron stars in the postmerger phase of binary neutron star coalescence. The universality of I -Q relations at nonzero temperature for fast rotating models, comparing a purely nuclear EoS with its counterparts containing hyperons or the entire baryon octet, respectively, is discussed, too. We find that the I -Q universality is broken in our models when thermal effects become important, independent on the presence of entropy gradients. Thus, the use of I -Q relations for the analysis of protoneutron stars or merger remnant data, including gravitational wave signals from the last stages of binary neutron star mergers, should be regarded with care.

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Unified treatment of subsaturation stellar matter at zero and finite temperature

Cited by 133 publications

References 106 publications

Crystallization of the inner crust of a neutron star and the influence of shell effects

Crystallization of the inner crust of a neutron star and the influence of shell effects

Crystallization of the outer crust of a non-accreting neutron star

New temperature dependent hyperonic equation of state: Application to rotating neutron star models and I−Q relations

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