Supernova explosions and the soft equation of state

Takahara, Mariko; Sato, Katsuhiko

doi:10.1086/166928

Cited by 42 publications

(23 citation statements)

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“…We note that the correlation between the transition densities and the maximum neutron star masses shown in Fig.4 follows the phenomenological discussions on phase transitions given in Ref. [53].…”

Section: Resultssupporting

confidence: 84%

Nucleons, nuclear matter and quark matter: a unified NJL approach

Lawley¹,

Bentz²,

Thomas³

2006

J. Phys. G: Nucl. Part. Phys.

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Section: Resultssupporting

confidence: 84%

Nucleons, nuclear matter and quark matter: a unified NJL approach

Lawley¹,

Bentz²,

Thomas³

2006

J. Phys. G: Nucl. Part. Phys.

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“…These results are consistent with other realistic core collapse simulations with other EOSs, which suggests that spherically symmetric core collapse supernova explosions are unlikely [1]. Furthermore, the central density of our stellar core following the bounce is higher than in the case of the Shen EOS because our EOS is softer, i.e., the present EOS is advantageous for supernova explosions [18,19,20].…”

Section: Introductionsupporting

confidence: 89%

Nuclear equation of state for core-collapse supernova simulations with realistic nuclear forces

et al. 2017

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A new table of the nuclear equation of state (EOS) based on realistic nuclear potentials is constructed for core-collapse supernova numerical simulations. Adopting the EOS of uniform nuclear matter constructed by two of the present authors with the cluster variational method starting from the Argonne v18 and Urbana IX nuclear potentials, the Thomas-Fermi calculation is performed to obtain the minimized free energy of a Wigner-Seitz cell in non-uniform nuclear matter. As a preparation for the Thomas-Fermi calculation, the EOS of uniform nuclear matter is modified so as to remove the effects of deuteron cluster formation in uniform matter at low densities. Mixing of alpha particles is also taken into account following the procedure used by Shen et al. ( , 2011. The critical densities with respect to the phase transition from non-uniform to uniform phase with the present EOS are slightly higher than those with the Shen EOS at small proton fractions. The critical temperature with respect to the liquid-gas phase transition decreases with the proton fraction in a more gradual manner than in the Shen * Corresponding author Email address: hajime.togashi@riken.jp (H. Togashi)Preprint submitted to Nuclear Physics A March 23, 2017EOS. Furthermore, the mass and proton numbers of nuclides appearing in non-uniform nuclear matter with small proton fractions are larger than those of the Shen EOS. These results are consequences of the fact that the density derivative coefficient of the symmetry energy of our EOS is smaller than that of the Shen EOS.

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“…The rebound of a larger mass in the gravitational potential implies a larger initial energy imparted to the outgoing shock wave. This initial shock energy has been found to depend sensitively on the stiffness of the equation of state around nuclear densities [94,101,102,15,103,104,39]. Unfortunately, most studies used the explosion energy of prompt hydrodynamic explosions to measure this effect.…”

Section: Hydrodynamicsmentioning

confidence: 99%