A NEW MULTI-DIMENSIONAL GENERAL RELATIVISTIC NEUTRINO HYDRODYNAMICS CODE FOR CORE-COLLAPSE SUPERNOVAE. II. RELATIVISTIC EXPLOSION MODELS OF CORE-COLLAPSE SUPERNOVAE

By Bernhard Müller, Hans-Thomas Janka, Andreas Marek. 2012

199 citations recorded by the source corpus.

We present the first two-dimensional general relativistic (GR) simulations of stellar core collapse and explosion with the CoCoNuT hydrodynamics code in combination with the Vertex solver for energy-dependent, three-flavor neutrino transport, using the extended conformal flatness condition for approximating the space–time metric and a ray-by-ray-plus ansatz to tackle the multi-dimensionality of the transport. For both of the investigated 11.2 and 15 M☉ progenitors we obtain successful, though seemingly marginal, neutrino-driven supernova explosions. This outcome and the time evolution of the models basically agree with results previously obtained with the Prometheus hydro solver including an approximative treatment of relativistic effects by a modified Newtonian potential. However, GR models exhibit subtle differences in the neutrinospheric conditions compared with Newtonian and pseudo-Newtonian simulations. These differences lead to significantly higher luminosities and mean energies of the radiated electron neutrinos and antineutrinos and therefore to larger energy-deposition rates and heating efficiencies in the gain layer with favorable consequences for strong nonradial mass motions and ultimately for an explosion. Moreover, energy transfer to the stellar medium around the neutrinospheres through nucleon recoil in scattering reactions of heavy-lepton neutrinos also enhances the mentioned effects. Together with previous pseudo-Newtonian models, the presented relativistic calculations suggest that the treatment of gravity and energy-exchanging neutrino interactions can make differences of even 50%–100% in some quantities and is likely to contribute to a finally successful explosion mechanism on no minor level than hydrodynamical differences between different dimensions.

Subfields: Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/d7c8f219c0fe50bc4538ec18460fc6e05652ecd1

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In Nuclear and High Energy Physics

Citations in the corpus

NEUTRINO-DRIVEN SUPERNOVA OF A LOW-MASS IRON-CORE PROGENITOR BOOSTED BY THREE-DIMENSIONAL TURBULENT CONVECTION (2015, background): “…pressure behind the shock (e.g., Herant et al. 1994; Burrows et al. 1995; Janka & Müller 1996; Murphy & Burrows 2008; Murphy et al. 2013; Marek & Janka 2009; Müller et al. 2012a,b, 2013; Müller & Janka 2014a,b; Suwa et al. 2013; Bruenn et al. 2013, 2014; Takiwaki et al. 2014; Couch & Ott 2014).”
Three-dimensional neutrino-driven supernovae: neutron star kicks, spins, and asymmetric ejection of nucleosynthesis products (2012, background): “…Ye in the neutrino-heated ejecta, while more sophisticated energy-dependent neutrino transport yields (slightly) proton-rich conditions in the neutrino-processed material expelled during the early explosion (e.g., Pruet et al. 2006; Fröhlich et al. 2006; Fischer et al. 2010; Müller et al. 2012).”
SELF-SUSTAINED ASYMMETRY OF LEPTON-NUMBER EMISSION: A NEW PHENOMENON DURING THE SUPERNOVA SHOCK-ACCRETION PHASE IN THREE DIMENSIONS (2014, methodology): “…the observable flux, here the number-flux N, from the ray-by-ray-computed number-flux densities, Fn(R), at points R on the radiating surface by an integration over the visible hemisphere, compare to Equation (7) in Müller et al. (2012): N (t) = 2 ∫ vis.hem. dA cos ϑ Fn(R, t) ( 1 + 3 2 cos ϑ ) .”
SASI ACTIVITY IN THREE-DIMENSIONAL NEUTRINO-HYDRODYNAMICS SIMULATIONS OF SUPERNOVA CORES (2013, methodology): “…in the work of Ott et al. (2012) the mean energy of the radiated electron neutrinos around 100ms after core bounce is more than 60% higher than that found with the Vertex transport code by Müller et al. (2012a), although both groups investigated the same 27M⊙ progenitor with relativistic methods.”
GENERAL-RELATIVISTIC SIMULATIONS OF THREE-DIMENSIONAL CORE-COLLAPSE SUPERNOVAE (2012, methodology): “…the simulation of B. Müller et al. (2012a) and the ones presented here, the key difference relevant for the development of neutrino-driven convection in our simulations is our choice of a Cartesian AMR grid as opposed to the spherical polar grid of the axisymmetric code of B. Müller et al. (2012a).”
PROGENITOR-EXPLOSION CONNECTION AND REMNANT BIRTH MASSES FOR NEUTRINO-DRIVEN SUPERNOVAE OF IRON-CORE PROGENITORS (2012, background): “…to note, however, that the relatively early explosions of the 11.2M⊙ and 27M⊙ progenitors of our model set and the later explosion of progenitors around 15M⊙ are fully compatible with recent results of 2D models with sophisticated neutrino transport (cf. Marek & Janka 2009; Müller et al. 2012a,b).”
MAGNETOROTATIONAL CORE-COLLAPSE SUPERNOVAE IN THREE DIMENSIONS (2014, background): “Typical O(1)B SNe may be driven by the neutrino mechanism (Bethe & Wilson 1985), in which neutrinos emitted from the collapsed core deposit energy behind the stalled shock, eventually driving it outward (e.g., Müller et al. 2012; Bruenn et al. 2013).”
THE DEVELOPMENT OF EXPLOSIONS IN AXISYMMETRIC AB INITIO CORE-COLLAPSE SUPERNOVA SIMULATIONS OF 12–25 M ⊙ ?> STARS (2012, methodology): “…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).”