Symmetry energy impact in simulations of core-collapse supernovae

By Tobias Fischer, M. Hempel, Irina Sagert, Y. Suwa, J. Schaffner-Bielich. 2013

133 citations recorded by the source corpus.

We present a review of a broad selection of nuclear matter equations of state (EOSs) applicable in core-collapse supernova studies. The large variety of nuclear matter properties, such as the symmetry energy, which are covered by these EOSs leads to distinct outcomes in supernova simulations. Many of the currently used EOS models can be ruled out by nuclear experiments, nuclear many-body calculations, and observations of neutron stars. In particular the two classical supernova EOS describe neutron matter poorly. Nevertheless, we explore their impact in supernova simulations since they are commonly used in astrophysics. They serve as extremely soft and stiff representative nuclear models. The corresponding supernova simulations represent two extreme cases, e.g., with respect to the protoneutron star (PNS) compactness and shock evolution. Moreover, in multi-dimensional supernova simulations EOS differences have a strong effect on the explosion dynamics. Because of the extreme behaviors of the classical supernova EOSs we also include DD2, a relativistic mean field EOS with density-dependent couplings, which is in satisfactory agreement with many current nuclear and observational constraints. This is the first time that DD2 is applied to supernova simulations and compared with the classical supernova EOS. We find that the overall behaviour of the latter EOS in supernova simulations lies in between the two extreme classical EOSs. As pointed out in previous studies, we confirm the impact of the symmetry energy on the electron fraction. Furthermore, we find that the symmetry energy becomes less important during the post-bounce evolution, where conversely the symmetric part of the EOS becomes increasingly dominating, which is related to the high temperatures obtained. Moreover, we study the possible impact of quark matter at high densities and light nuclear clusters at low and intermediate densities.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/15e02e703ab49175baa289d2980fe4e82d3fa2bc

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Citations in the corpus

The Nuclear Symmetry Energy (2016, background): “Since the collapse evolution is mainly determined by the electron capture process on nuclei, these EOS give different [121] rate of deleptonization (i.”
Dynamical Mass Ejection from Binary Neutron Star Mergers (2016, result): “This equation of state is broadly consistent with observations, but falls outside the favored region of microscopic neutron matter calculations (e.g., Fischer et al. 2014).”
NEW HYPERON EQUATIONS OF STATE FOR SUPERNOVAE AND NEUTRON STARS IN DENSITY-DEPENDENT HADRON FIELD THEORY (2014, methodology): “(12) In this work we employ the DD2 parameter set (Typel et al. 2010; Fischer et al. 2014), where the coefficients in Equations (11) and (12), the saturation density, the nucleon-meson couplings at the saturation density, and the mass of σ mesons are determined by fitting the properties of finite…”
The Gravitational Wave Signal from Core-collapse Supernovae (2018, methodology): “In our models, we use three different equations of state (EOS), namely, the SFHo EOS (Steiner et al. 2013), the Lattimer-Swesty EOS with nuclear incompressibility parameter 220 MeV (Lattimer & Swesty 1991), and the DD2 EOS (Fischer et al. 2014; Banik et al. 2014).”
Revisiting the SN1987A gamma-ray limit on ultralight axion-like particles (2014, background): “Note further that we neglect contributions from protons bound in nuclei for the ALP production rate; in particular light clusters but also heavy clusters become abundant at low temperatures and densities [60].”
Symmetry Parameter Constraints from a Lower Bound on Neutron-matter Energy (2016, methodology): “The symmetry energy is also important in calculations of the r-process (Mumpower et al. 2016), supernovae (Fischer et al. 2014), and neutron-star mergers (Bauswein et al. 2016).”
What can be learned from a future supernova neutrino detection (2017, background): “(ii) the neutrino spectra emitted at the neutrinosphere are sensitive to fundamental physics of the nuclear equation-of-state [40, 41, 42, 43, 44, 45, 46, 47, 48], general relativity [34, 49], and in-medium nuclear effects [50, 51, 52], and (iii) we have also learned that the neutrino flavor composi”