Enforcing causality in nonrelativistic equations of state at finite temperature

Constantinou, Constantinos; Prakash, Madappa

doi:10.1103/physrevc.95.055802

Cited by 6 publications

(8 citation statements)

References 53 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…( 2) and (3). We have confirmed that it is always possible to modify the high-density equation of state (n > 2n 0 ) in our generated samples in order to reach a maximum mass of 2.0 M while imposing sub-luminal speeds of sound [108,109]. In this work, however, we consider the energy density functional as in Eqs.…”

Section: Resultsmentioning

confidence: 77%

Bayesian modeling of the nuclear equation of state for neutron star tidal deformabilities and GW170817

Lim¹,

Holt²

2019

Eur. Phys. J. A

View full text Add to dashboard Cite

We present predictions for neutron star tidal deformabilities obtained from a Bayesian analysis of the nuclear equation of state, assuming a minimal model at high-density that neglects the possibility of phase transitions. The Bayesian posterior probability distribution is constructed from priors obtained from microscopic many-body theory based on realistic two-and three-body nuclear forces, while the likelihood functions incorporate empirical information about the equation of state from nuclear experiments. The neutron star crust equation of state is constructed from the liquid drop model, and the core-crust transition density is found by comparing the energy per baryon in inhomogeneous matter and uniform nuclear matter. From the cold β -equilibrated neutron star equation of state, we then compute neutron star tidal deformabilities as well as the mass-radius relationship. Finally, we investigate correlations between the neutron star tidal deformability and properties of finite nuclei.

show abstract

Section: Resultsmentioning

confidence: 77%

Bayesian modeling of the nuclear equation of state for neutron star tidal deformabilities and GW170817

Lim¹,

Holt²

2019

Eur. Phys. J. A

View full text Add to dashboard Cite

show abstract

“…Nevertheless, the modifications can be useful for studying the impact of a higher maximum NS mass on astrophysical simulations while keeping the properties of saturation-density nuclear matter fixed. A thermodynamically consistent method to modify nonrelativistic equations of state so that they respect causality at high densities has recently been suggested [87]. We postpone its implementation to future work.…”

Section: High-density Eos Modificationsmentioning

confidence: 99%

Open-source nuclear equation of state framework based on the liquid-drop model with Skyrme interaction

2017

View full text Add to dashboard Cite

The equation of state (EOS) of dense matter is an essential ingredient for numerical simulations of core-collapse supernovae and neutron star mergers. The properties of matter near and above nuclear saturation density are uncertain, which translates into uncertainties in astrophysical simulations and their multimessenger signatures. Therefore, a wide range of EOSs spanning the allowed range of nuclear interactions are necessary for determining the sensitivity of these astrophysical phenomena and their signatures to variations in input microphysics. We present a new set of finite temperature EOSs based on experimentally allowed Skyrme forces. We employ a liquid-drop model of nuclei to capture the nonuniform phase of nuclear matter at subsaturation density, which is blended into a nuclear statistical equilibrium EOS at lower densities. We also provide a new, open-source code for calculating EOSs for arbitrary Skyrme parametrizations. We then study the effects of different Skyrme parametrizations on thermodynamical properties of dense astrophysical matter, the neutron star mass-radius relationship, and the core collapse of 15 and 40 solar mass stars.

show abstract

“…Often, the density at which causality is violated lies within the central densities of neutron stars. Although a method to impose causality based on thermodynamical arguments has been known for a while for cold stars [52,53], it is only recently that a similar method has been devised at finite temperature [54]. A practical way to avoid this problem is to screen repulsive contributions from higher-than-two-body interactions (as they lead to an energy per particle that varies faster than linearly at high density) as in Refs.…”

Section: The Supra-nuclear Equation Of Statementioning

confidence: 99%

Dense matter equation of state for neutron star mergers

et al. 2019

View full text Add to dashboard Cite

In simulations of binary neutron star mergers, the dense matter equation of state (EOS) is required over wide ranges of density and temperature as well as under conditions in which neutrinos are trapped, and the effects of magnetic fields and rotation prevail. Here we assess the status of dense matter theory and point out the successes and limitations of approaches currently in use. A comparative study of the excluded volume (EV) and virial approaches for the npα system using the equation of state of Akmal, Pandharipande and Ravenhall for interacting nucleons is presented in the sub-nuclear density regime. Owing to the excluded volume of the α-particles, their mass fraction vanishes in the EV approach below the baryon density 0.1 fm −3 , whereas it continues to rise due to the predominantly attractive interactions in the virial approach. The EV approach of Lattimer et al. is extended here to include clusters of light nuclei such as d, 3 H and 3 He in addition to α-particles. Results of the relevant state variables from this development are presented and enable comparisons with related but slightly different approaches in the literature. We also comment on some of the sweet and sour aspects of the supra-nuclear EOS. The extent to which the neutron star gravitational and baryon masses vary due to thermal effects, neutrino trapping, magnetic fields and rotation are summarized from earlier studies in which the effects from each of these sources were considered separately. Increases of about 20%( 50%) occur for rigid (differential) rotation with comparable increases occurring in the presence of magnetic fields only for fields in excess of 10 18 Gauss. Comparatively smaller changes occur due to thermal effects and neutrino trapping. Some future studies to gain further insight into the outcome of dynamical simulations are suggested. PACS. 26.60.-c Nuclear matter aspects of neutron stars -26.60.Kp Equations of state of neutron-star matter -97.60.-s Late stages of stellar evolution (including black holes) -97.80.-d Binary and multiple stars arXiv:1809.08126v2 [astro-ph.HE]

show abstract

Enforcing causality in nonrelativistic equations of state at finite temperature

Cited by 6 publications

References 53 publications

Bayesian modeling of the nuclear equation of state for neutron star tidal deformabilities and GW170817

Bayesian modeling of the nuclear equation of state for neutron star tidal deformabilities and GW170817

Open-source nuclear equation of state framework based on the liquid-drop model with Skyrme interaction

Dense matter equation of state for neutron star mergers

Contact Info

Product

Resources

About