Deducing the nuclear-matter incompressibility coefficient from data on isoscalar compression modes

By S. Shlomo, V. Kolomietz, G. Colò. 2006

261 citations recorded by the source corpus.

Subfields: Nuclear and High Energy Physics, Spectroscopy

View Paper: https://www.semanticscholar.org/paper/d21f8df30e429b60b11a1c45b4ee6ea44febc9e1

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In Nuclear and High Energy Physics

In Spectroscopy

Citations in the corpus

A NEW MULTI-DIMENSIONAL GENERAL RELATIVISTIC NEUTRINO HYDRODYNAMICS CODE FOR CORE-COLLAPSE SUPERNOVAE. II. RELATIVISTIC EXPLOSION MODELS OF CORE-COLLAPSE SUPERNOVAE (2012, background): “…EoS has raised some objections (Nordhaus et al. 2010; Dasgupta et al. 2012) because measurements point to K = 240 MeV for symmetric nuclear matter (Shlomo et al. 2006), and because observations have recently pushed the maximum neutron star mass to at least 2M⊙ (Demorest et al. 2010), which is…”
Two-Dimensional Multiangle, Multigroup Neutrino Radiation-Hydrodynamic Simulations of Postbounce Supernova Cores (2008, methodology): “1) of the normalized specific spectral neutrino intensityIν for electron neutrinos at 12.6 MeV.”
HADRON–QUARK CROSSOVER AND MASSIVE HYBRID STARS WITH STRANGENESS (2012, background): “This means an interesting possibility that we can reconcile the existence of massive neutron stars (M > 2M⊙) with the experimental nuclear incompressibility κ = (240±20)MeV (Shlomo et al. (2006)).”
Criteria for Core-Collapse Supernova Explosions by the Neutrino Mechanism (2008, result): “While this suggests an interesting dependence of explosion on the EOS, we note that laboratory experiments indicate that K = 240 ± 20 MeV (Shlomo et al. 2006; Lattimer & Prakash 2007), a value that is more consistent with the non-explosive model.”
Combined Constraints on the Equation of State of Dense Neutron-rich Matter from Terrestrial Nuclear Experiments and Observations of Neutron Stars (2018, background): “(Danielewicz et al. 2002; Shlomo et al. 2006; Chen et al. 2009; Steiner et al. 2010; Piekarewicz 2010; Khan et al. 2012; Dutra et al. 2012, 2014; Li & Han 2013; Colò et al. 2014; Cai & Chen 2014; Zhang et al. 2017).”
Symmetry Parameter Constraints from a Lower Bound on Neutron-matter Energy (2016, unknown): “The values of the saturation parameters are E0=−15.9±0.4MeV, n0= 0.164±0.007 fm−3 (Drischler et al. 2016b), and K0=240± 20MeV (Shlomo et al. 2006; Piekarewicz 2010) or K0=230± 40MeV (Khan et al. 2012).”
THREE-DIMENSIONAL HYDRODYNAMIC CORE-COLLAPSE SUPERNOVA SIMULATIONS FOR AN 11.2 M☉ STAR WITH SPECTRAL NEUTRINO TRANSPORT (2011, background): “Moreover, the softer nuclear equation of state (EOS), such as of the Lattimer & Swesty (1991) (LS) EOS with an incompressibility at nuclear densities,K, of 180 MeV, is employed in those simulations.”
NEW EQUATIONS OF STATE IN SIMULATIONS OF CORE-COLLAPSE SUPERNOVAE (2011, unknown): “The experiments probe nuclear matter slightly below saturation density and furthermore the deduced results depend on the nuclear interactions (e.g., the behavior of the symmetry energy) which are taken for the data analysis (see, e.g., Shlomo et al. (2006); Piekarewicz (2004); Sharma (2009)).”
Multiple physical elements to determine the gravitational-wave signatures of core-collapse supernovae (2011, background): “On top of a striking evidence that favors a sti ffer EOS based on the nuclear experimental data ( K = 240± 20 MeV, [202]), the soft EOS may not account for the recently observed massive neutron star of ∼ 2M⊙ [203] [see the maximum mass for the LS180 EOS in 204, 205].”