Postbounce Evolution of Core-Collapse Supernovae: Long-Term Effects of the Equation of State

By K. Sumiyoshi, S. Yamada, Hideyuki Suzuki, Hong Shen, S. Chiba, Hiroshi Toki. 2005

219 citations recorded by the source corpus.

We study the evolution of a supernova core from the beginning of the gravitational collapse of a 15 M☉ star up to 1 s after core bounce. We present results of spherically symmetric simulations of core-collapse supernovae by solving general relativistic ν-radiation hydrodynamics in the implicit time differencing. We aim to explore the evolution of shock waves in the long term and investigate the formation of proto-neutron stars together with supernova neutrino signatures. These studies are done to examine the influence of the equation of state (EOS) on the postbounce evolution of shock waves in the late phase and the resulting thermal evolution of proto-neutron stars. We compare two sets of EOSs, namely, those by Lattimer and Swesty (LS-EOS) and by Shen et al. (SH-EOS). We found that, for both EOSs, the core does not explode and the shock wave stalls similarly in the first 100 ms after bounce. A revival of the shock wave does not occur even after a long period in either case. However, the recession of the shock wave appears different beyond 200 ms after bounce, having different thermal evolution of the central core. A more compact proto-neutron star is found for LS-EOS than SH-EOS with a difference in the central density by a factor of ~2 and a difference of ~10 MeV in the peak temperature. The resulting spectra of supernova neutrinos are different to an extent that may be detectable by terrestrial neutrino detectors.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/1f19c508a33cf5e95b48c8bafe52331ec78283a4

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Citations in the corpus

On the Normalization of the Cosmic Star Formation History (2006, result): “As found and discussed in Yüksel et al. (2005), our results favour effective temperatures at the lower end of the predicted range (Keil et al. 2003; Thompson et al. 2003; Liebendoerfer et al. 2005; Sumiyoshi et al. 2005).”
NUCLEOSYNTHESIS IN ELECTRON CAPTURE SUPERNOVAE OF ASYMPTOTIC GIANT BRANCH STARS (2008, background): “…Germany; thj@mpa-garching.mpg.de, kitaura@mpa-garching.mpg.de help of multi-dimensional effects (Rampp & Janka 2000; Mezzacappa et al. 2001; Liebendörfer et al. 2001; Thompson et al. 2003; Sumiyoshi et al. 2005; Buras et al. 2006), at least for standard nuclear and neutrino physics input.”
The Status of Multi-Dimensional Core-Collapse Supernova Models (2016, background): “…demonstrated that the neutrino-driven mechanism is not viable in spherical symmetry (Rampp & Janka 2000, 2002; Liebendörfer et al. 2001, 2004, 2005; Sumiyoshi et al. 2005; Buras et al. 2006a,b; Müller et al. 2010; Fischer et al. 2010; Lentz et al. 2012a,b), except for supernova progenitors of…”
A COMPARISON OF TWO- AND THREE-DIMENSIONAL NEUTRINO-HYDRODYNAMICS SIMULATIONS OF CORE-COLLAPSE SUPERNOVAE (2013, background): “In the long history, a very important lesson we have learned from Rampp & Janka (2000); Liebendörfer et al. (2001); Thompson et al. (2003); Sumiyoshi et al. (2005) near the Millennium, is that the spherically-symmetric (1D) form of this mechanism fails to explode canonical massive stars.”
AN OPEN-SOURCE NEUTRINO RADIATION HYDRODYNAMICS CODE FOR CORE-COLLAPSE SUPERNOVAE (2014, methodology): “This has been done in spherical symmetry (Mezzacappa & Bruenn 1993c,a,b; Liebendörfer et al. 2005; Sumiyoshi et al. 2005), in 2D (Livne et al. 2004; Ott et al. 2008; Brandt et al. 2011), and recently in 3D (Sumiyoshi & Yamada 2012; Sumiyoshi et al. 2014).”
Two-dimensional hydrodynamic core-collapse supernova simulations with spectral neutrino transport II. Models for different progenitor stars (2005, result): “We therefore found explosionsof these stars neither in spherical symmetry (in agreement with Liebendörfer et al. 2002, Thompson et al. 2003, Sumiyoshi et al. 2005) nor in 2D.”
THE DEVELOPMENT OF EXPLOSIONS IN AXISYMMETRIC AB INITIO CORE-COLLAPSE SUPERNOVA SIMULATIONS OF 12–25 M ⊙ ?> STARS (2012, background): “…drawn from these and other 1D studies is that neutrinos alone cannot power CCSNe in spherical symmetry, yet 1D simulations do remain a vital guide to the remaining CCSN physics at low computational cost (e.g., Thompson et al. 2003; Sumiyoshi et al. 2005; Lentz et al. 2012c,b; Müller et al. 2012b).”
THE ISOTROPIC DIFFUSION SOURCE APPROXIMATION FOR SUPERNOVA NEUTRINO TRANSPORT (2007, background): “Spherical symmetry is much better treated with three-flavour Boltzmann transport where the comprehensive equations of radiative transfer can consistently be solved (Rampp & Janka 2002; Thompson et al. 2003; Liebendörfer et al. 2004; Sumiyoshi et al. 2005).”
THREE-DIMENSIONAL HYDRODYNAMIC CORE-COLLAPSE SUPERNOVA SIMULATIONS FOR AN 11.2 M☉ STAR WITH SPECTRAL NEUTRINO TRANSPORT (2011, background): “However, one important lesson we have learned from Rampp & Janka (2000); Liebendörfer et al. (2001); Thompson et al. (2003); Sumiyoshi et al. (2005) who implemented the best input physics and numerics to date, is that the mechanism fails to blow up canonical massive stars in spherical symmetric…”
What can be learned from a future supernova neutrino detection (2017, background): “O’Connor & Ott [155] did to produce figure (4), and similarly differences due to the Equation of State are routinely determined by using multiple different forms [41].”
GENERAL-RELATIVISTIC SIMULATIONS OF THREE-DIMENSIONAL CORE-COLLAPSE SUPERNOVAE (2012, background): “…full Boltzmann neutrino transport have shown that neutrino heating alone fails to drive an explosion in all but the lowest-mass massive stars (Liebendörfer et al. 2001; Rampp & Janka 2002; Thompson et al. 2003; Sumiyoshi et al. 2005; Kitaura et al. 2006; Hüdepohl et al. 2010; Burrows et al. 2007a).”
A Survey About Nothing: Monitoring a Million Supergiants for Failed Supernovae (2008, background): “Despite intense theoretical and computational efforts (in 1D, e.g., Rampp & Janka 2000; Liebendörfer et al. 2001; Thompson et al. 2003; Sumiyoshi et al. 2005; in 2D: e.g., Fryer 1999; Buras et al. 2003, 2006; Livne et al. 2004; Ohnishi et al. 2006; and in 3D: e.g., Fryer & Warren 2002) it is…”