The role of the equation of state in the 'prompt' phase of type II supernovae

Swesty, F. Douglas; Lattimer, James M.; Myra, E. S.

doi:10.1086/173974

Cited by 92 publications

(95 citation statements)

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“…Janka et al 2005;Sumiyoshi et al 2005), agree with the results obtained in the 1980s and 1990s (e.g. Myra & Bludman 1989;Swesty et al 1994). Namely, the prompt shock is not able to drive a supernova explosion, except in the case of small iron cores (Baron & Cooperstein 1990) or very soft equations of state (Baron et al 1987).…”

Section: Introductionsupporting

confidence: 88%

Effects of the temperature dependence of the in-medium nucleon mass on core-collapse supernovae

Fantina

Blottiau

Margueron

et al. 2012

A&A

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Aims. A complete description of the core collapse supernova mechanism requires an appropriate treatment of both the hydrodynamics and the microphysics. We study the influence of a nuclear physics input, namely the temperature dependence of the nucleon effective mass in nuclei induced by the in-medium effects, in the core collapse of a massive star. Methods. We present here the first implementation of this nuclear input in a hydrodynamical one-dimensional simulation. The simulations are performed with a spherically symmetric Newtonian model, with neutrino transport treated in the multi-group flux-limited diffusion approximation. Results. The inclusion of the temperature dependence of the in-medium nucleon mass has an impact on the equation of state of the system and reduces the deleptonisation during the collapse. This results in a non-negligible effect on the shock wave energetics. The shock wave is formed more outwards, and in the first few milliseconds after bounce the shock front has propagated further out.

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Section: Introductionsupporting

confidence: 88%

Effects of the temperature dependence of the in-medium nucleon mass on core-collapse supernovae

Fantina

Blottiau

Margueron

et al. 2012

A&A

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“…There is general agreement now, supported by a large number of numerical calculations (e.g., Bruenn 1985;Bruenn 1989a;Bruenn 1989b;Myra et al 1987;Myra & Bludman 1989;Swesty, Lattimer, & Myra 1994), that this energy is not sufficient for the shock to reach the surface of the iron core: The energy losses from behind the shock by photodisintegration of nuclei to α-particles and free nucleons (∼ 1.5 × 10 51 erg per 0.1 M ) as well as neutrino escape after shock breakout through the neutrinosphere (some 10 51 erg) are so severe that the shock stalls within milliseconds. Only in case of extremely small iron cores (M < ∼ 1.1 M ; Baron & Cooperstein 1990) or an extraordinarily soft nuclear EoS (Baron, Cooperstein, & Kahana 1985;Baron et al 1987) is the prompt hydrodynamical shock able to disrupt the star.…”

Section: Hydrodynamical (Prompt) Mechanismmentioning

confidence: 68%

Explosion Mechanisms of Massive Stars

Janka

Buras

Kifonidis

et al. 2004

Astrophysics and Space Science Library

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One of the central problems in supernova theory is the question how massive stars explode. Understanding the physical processes that drive the explosion is crucial for linking the stellar progenitors to the final remnants and for predicting observable properties like explosion energies, neutron star and black hole masses, nucleosynthetic yields, explosion anisotropies, and pulsar kicks. In this article we review different suggestions for the explosion mechanism and discuss the constraints that can or cannot be deduced from observations. The prompt hydrodynamical bounce-shock mechanism has turned out not to work for typical stellar iron cores and empirical values of the compressibility of bulk nuclear matter. Magnetohydrodynamical models on the other hand contain a number of imponderabilities and are still far behind the level of refinement that has been achieved in nonmagnetic simulations. In view of these facts the neutrino-driven mechanism must still be considered as the standard paradigm to explain the explosion of ordinary supernovae, although its viability has yet to be demonstrated convincingly.Since spherically symmetric models do not yield explosions, the hope rests on the helpful effects of convection inside the nascent neutron star, which could boost the neutrino luminosity, and convective overturn in the neutrino-heated region behind the stalled shock, which increases the efficiency of neutrino-energy transfer in this layer. Here we present the first two-dimensional simulations of these processes which have been 1

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“…The expected neutrino signal from gravitational collapse supernovae within our Galaxy is sensitive to the symmetry energy both before core bounce (Swesty et al 1994) and at later times during the proto-neutron-star stage (Roberts et al 2012). The symmetry energy near n s , the baryon density at saturation, determines the radii (Lattimer & Prakash 2001) of neutron stars.…”

Section: Introductionmentioning

confidence: 98%

Constraining the Symmetry Parameters of the Nuclear Interaction

Lattimer

Lim

2013

ApJ

Self Cite

565

629

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One of the major uncertainties in the dense matter equation of state has been the nuclear symmetry energy. The density dependence of the symmetry energy is important in nuclear astrophysics, as it controls the neutronization of matter in core-collapse supernovae, the radii of neutron stars and the thicknesses of their crusts, the rate of cooling of neutron stars, and the properties of nuclei involved in r-process nucleosynthesis. We show that fits of nuclear masses to experimental masses, combined with other experimental information from neutron skins, heavy ion collisions, giant dipole resonances, and dipole polarizabilities, lead to stringent constraints on parameters that describe the symmetry energy near the nuclear saturation density. These constraints are remarkably consistent with inferences from theoretical calculations of pure neutron matter, and, furthermore, with astrophysical observations of neutron stars. The concordance of experimental, theoretical, and observational analyses suggests that the symmetry parameters S v and L are in the range 29.0-32.7 MeV and 40.5-61.9 MeV, respectively, and that the neutron star radius, for a 1.4 M star, is in the narrow window 10.7 km < R < 13.1 km (90% confidence). We can also set tight limits to the size of neutron star crusts and the fractional moment of inertia they contain, as well as the overall moment of inertia and quadrupole polarizability of 1.4 M stars. Our results also have implications for the disk mass and ejected mass of compact mergers involving neutron stars.

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The role of the equation of state in the 'prompt' phase of type II supernovae

Cited by 92 publications

References 0 publications

Effects of the temperature dependence of the in-medium nucleon mass on core-collapse supernovae

Effects of the temperature dependence of the in-medium nucleon mass on core-collapse supernovae

Explosion Mechanisms of Massive Stars

Constraining the Symmetry Parameters of the Nuclear Interaction

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