Composition and thermodynamics of nuclear matter with light clusters

By S. Typel, G. Röpke, T. Klähn, David B. Blaschke, H. Wolter. 2009

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We investigate nuclear matter at a finite temperature and density, including the formation of light clusters up to the alpha particle (1<=A<=4). The novel feature of this work is to include the formation of clusters as well as their dissolution due to medium effects in a systematic way using two many-body theories: a microscopic quantum statistical (QS) approach and a generalized relativistic mean-field (RMF) model. Nucleons and clusters are modified by medium effects. While the nucleon quasiparticle properties are determined within the RMF model from the scalar and vector self-energies, the cluster binding energies are reduced because of Pauli blocking shifts calculated in the QS approach. Both approaches reproduce the limiting cases of nuclear statistical equilibrium (NSE) at low densities and cluster-free nuclear matter at high densities. The treatment of the cluster dissociation is based on the Mott effect due to Pauli blocking, implemented in slightly different ways in the QS and the generalized RMF approaches. This leads to somewhat different results in the intermediate density range of about 10{sup -3} to 10{sup -1} fm{sup -3}, which gives an estimate of the present accuracy of the theoretical predictions. We compare the numerical results of these models for cluster abundances andmore » thermodynamics in the region of medium excitation energies with temperatures T<=20 MeV and baryon number densities from zero to a few times saturation density. The effects of cluster formation on the liquid-gas phase transition and on the density dependence of the symmetry energy are studied. It is demonstrated that the parabolic approximation for the asymmetry dependence of the nuclear equation of state breaks down at low temperatures and at subsaturation densities because of cluster formation. Comparison is made with other theoretical approaches, in particular, those that are commonly used in astrophysical calculations. The results are relevant for heavy-ion collisions and astrophysical applications.« less

Subfields: Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/6bdd40d03e4a09d9be6dec9dcd96bc679c02d3a5

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Citations in the corpus

Gravitational waves and non-axisymmetric oscillation modes in mergers of compact object binaries (2011, background): “Though to date several finite-temperature EOSs (Typel et al. 2010; Hempel & Schaffner-Bielich 2010; Shen etal.”
Superfluidity in nuclear systems and neutron stars (2018, background): “It has been also speculated that deuteron condensates can be formed in the dilute nuclear matter found in supernova and hot proto-neutron-star matter at sub-saturation densities; see for example [176, 274–282].”
Maximum mass, moment of inertia and compactness of relativistic stars (2016, unknown): “…L, Pandharipande & Smith (1975); HS DD2, HS NL3, HS TM1, HS TMA, SFHo, SFHx, Gaitanos et al. (2004); Hempel, M. and Schaffner-Bielich, J. (2010); Typel et al. (2010); c© 0000 RAS, MNRAS 000, 1–12 GShen-NL3, Shen et al. (2010), the Walecka model [EOS-O, Arnett & Bowers (1977)] and the…”
Neutron-powered precursors of kilonovae (2014, methodology): “This calculation was performed by using a nuclear reaction network to post-process SPH trajectories extracted from the 1.35-1.35M⊙ NS binary merger simulation of Bauswein et al. (2013) that employed the DD2 equation of state (Typel et al. 2010; Hempel & Schaffner-Bielich 2010).”
A new quark-hadron hybrid equation of state for astrophysics - I. High-mass twin compact stars (2014, methodology): “See Typel et al. (2010) for the definition of the quantities in the table and their relation to the coupling functions.”
Symmetry energy impact in simulations of core-collapse supernovae (2013, methodology): “gs. The DD2 EOS has an excellent qualitative and quantitative agreement with Chiral EFT across all densities. Note that the parameterization DD, which is basically identical to DD2, (for details, see [67,25]) has been introduced long before any of these constraints became available at the current pr”
GW170817: Joint Constraint on the Neutron Star Equation of State from Multimessenger Observations (2017, methodology): “…and we adopt four temperature and composition dependent nuclear EOSs spanning the range of the nuclear uncertainties: the DD2 EOS (Hempel & Schaffner-Bielich 2010; Typel et al. 2010), the BHBΛf EOS (Banik et al. 2014), the LS220 EOS (Lattimer & Swesty 1991), and the SFHo EOS (Steiner et al. 2013).”
Binary Neutron Star Mergers: Mass Ejection, Electromagnetic Counterparts, and Nucleosynthesis (2018, methodology): “For our survey we consider four different nuclear EOSs: the DD2 EOS (Hempel & Schaffner-Bielich 2010; Typel et al. 2010), the BHBΛf EOS (Banik et al. 2014), the LS220 EOS (Lattimer & Swesty 1991), and the SFHo EOS (Steiner et al. 2013).”
NEW EQUATIONS OF STATE IN SIMULATIONS OF CORE-COLLAPSE SUPERNOVAE (2011, methodology): “Typel et al. (2010) use a generalized RMF and a quantum statistical model (Röpke 2011) to study supernova matter taking into account the most important light nuclei with mass number A ≤ 4.”
Comprehensive nucleosynthesis analysis for ejecta of compact binary mergers (2014, background): “…employed microphysical EOSs are SFHO, SFHX (Steiner, Hempel & Fischer 2013), TM1 (Sugahara & Toki 1994; Hempel et al. 2012), TMA (Toki et al. 1995; Hempel et al. 2012), and DD2 (Hempel & Schaffner-Bielich 2010; Typel et al. 2010), which are all derived within the relativistic mean-field approach.”