Dense Nuclear Matter Equation of State from Heavy-Ion Collisions

Sorensen, Agnieszka; Agarwal, Kshitij; Brown, K; Chajęcki, Z.; Danielewicz, P; Lynch, W; Pratt, S; Tsang, M; Drischler, C; Gandolfi, Stefano; Tews, Ingo; Holt, Jocelyn R.; Ko, C. M.; Kaminski, Matthias; Kumar, R; Li, B; Newton, William; McIntosh, Alex; Savchuk, O; Vogt, R.; Wolter, H.H.; Zbroszczyk, H.

doi:10.2172/1959612

“…However, a more complete picture of the phase structure of QCD for asymmetric matter at zero temperature will require constraints from both astrophysical observations and laboratory measurements, as well as input from effective theories and pQCD (for a detailed discussions see Refs. [32,33]).…”

Section: Discussionmentioning

confidence: 99%

Searching for phase transitions in neutron stars with modified Gaussian processes

Mroczek

¹

,

Miller

²

,

Jacquelyn

³

et al. 2023

J. Phys.: Conf. Ser.

4

0

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Gaussian processes provide a promising framework by which to extrapolate the equation of state (EoS) of cold, catalyzed matter beyond 1 – 2 times nuclear saturation density. Here we discuss how to extend Gaussian processes to include nontrivial features in the speed of sound, such as bumps, kinks, and plateaus, which are predicted by nuclear models with exotic degrees of freedom. Using a fully Bayesian analysis incorporating measurements from X-ray sources, gravitational wave observations, and perturbative QCD results, we show that these features are compatible with current constraints and report on how the features affect the EoS posteriors.

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“…It should be pointed out that microscopic transport models are essential for the extraction of the EOS based on data from collision experiments. Various theoretical approaches to study the dynamics of such collisions and to define sensitive observables are pursued [282,283], and a continued effort exists aiming at reducing the model uncertainties [284]. An important aspect is the relevance of the isospin degree of freedom for the EOS once the temperature in the fireball reaches a significant fraction of the pion mass.…”

Section: Future Developmentsmentioning

confidence: 99%

Nuclear structure opportunities with GeV radioactive beams at FAIR

Aumann,

Bertulani,

Duer

et al. 2024

Phil. Trans. R. Soc. A.

0

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The Facility for Antiproton and Ion Research (FAIR) is in its final construction stage next to the campus of the Gesellschaft für Schwerionenforschung Helmholtzzentrum for heavy-ion research in Darmstadt, Germany. Once it starts its operation, it will be the main nuclear physics research facility in many basic sciences and their applications in Europe for the coming decades. Owing to the ability of the new fragment separator, Super-FRagment Separator, to produce high-intensity radioactive ion beams in the energy range up to about 2 GeV/nucleon, these can be used in various nuclear reactions. This opens a unique opportunity for various nuclear structure studies across a range of fields and scales: from low-energy physics via the investigation of multi-neutron systems and halos to high-density nuclear matter and the equation of state, following heavy-ion collisions, fission and study of short-range correlations in nuclei and hypernuclei. The newly developed reactions with relativistic radioactive beams (R 3 B) set up at FAIR would be the most suitable and versatile for such studies. An overview of highlighted physics cases foreseen at R 3 B is given, along with possible future opportunities, at FAIR. This article is part of the theme issue ‘The liminal position of Nuclear Physics: from hadrons to neutron stars’.

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“…To test our mass and radius scalings, shown in Figure 1 are the R max -ν c (upper panel) and M NS max -Γ c (lower panel) correlations, using 87 phenomenological and 17 extra microscopic NS EOSs with and/or without considering hadron- quark phase transitions and hyperons by solving numerically the original TOV equations. The phenomenological EOSs are from three rather different classes of EOS models (Iida & Sato 1997): the covariant relativistic mean-field (RMF) models (Serot & Walecka 1986) and the nonrelativistic energy density functionals (EDFs) of the Gogny-like type (Cai & Li 2022) as well as the conventional Skyrme type (Vautherin & Brink 1972;Stone & Reinhard 2007;Zhang & Chen 2016). Within each EOS class, different EOS models are generated by perturbing the model coupling constants within their empirical uncertain ranges.…”

Section: Validations Of Ns Radius/mass Scalings By Solving the Origin...mentioning

confidence: 99%

“…Understanding the nature and Equation of State (EOS) of supradense matter in neutron stars (NSs) (Walecka 1974;Collins & Perry 1975;Chin 1977;Freedman & McLerran 1977a, 1977b, 1977cWiringa et al 1988;Akmal et al 1998) has been a longstanding and shared goal of both astrophysics and nuclear physics (Shuryak 1980;Lattimer & Prakash 2001;Danielewicz et al 2002;Alford et al 2008;Li et al 2008;Özel & Freire 2016;Watts et al 2016;Oertel et al 2017;Baym et al 2018;Vidaña 2018;Baiotti 2019;Orsaria et al 2019;Dexheimer et al 2021;Lattimer 2021;Lovato et al 2022;Sorensen et al 2023). In particular, novel phases and new degrees of freedom are expected to appear in NS cores where the density is the highest.…”

Section: Introductionmentioning

confidence: 99%

Core States of Neutron Stars from Anatomizing Their Scaled Structure Equations

Cai¹,

Li

²

,

Zhang³

2023

ApJ

Self Cite

5

0

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Given an Equation of State (EOS) for neutron star (NS) matter, there is a unique mass–radius sequence characterized by a maximum mass M NS max at radius R max. We first show analytically that the M NS max and R max scale linearly with two different combinations of the NS central pressure P c and energy density ε c, by dissecting perturbatively the dimensionless Tolman–Oppenheimer–Volkoff (TOV) equations governing NS internal variables. The scaling relations are then verified via 87 widely used and rather diverse phenomenological as well as 17 microscopic NS EOSs with/without considering hadron–quark phase transitions and hyperons, by solving numerically the original TOV equations. The EOS of the densest NS matter allowed before it collapses into a black hole is then obtained. Using the universal M NS max and R max scalings and Neutron Star Interior Composition Explorer and XMM-Newton mass–radius observational data for PSR J0740+6620, a very narrow constraining band on the NS central EOS is extracted directly from the data for the first time, without using any specific input EOS model.

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Dense Nuclear Matter Equation of State from Heavy-Ion Collisions

Cited by 9 publications

References 0 publications

Searching for phase transitions in neutron stars with modified Gaussian processes

Searching for phase transitions in neutron stars with modified Gaussian processes

Nuclear structure opportunities with GeV radioactive beams at FAIR

Core States of Neutron Stars from Anatomizing Their Scaled Structure Equations

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