NEW TWO-DIMENSIONAL MODELS OF SUPERNOVA EXPLOSIONS BY THE NEUTRINO-HEATING MECHANISM: EVIDENCE FOR DIFFERENT INSTABILITY REGIMES IN COLLAPSING STELLAR CORES

By Bernhard Müller, Hans-Thomas Janka, Alexander Heger. 2012

141 citations recorded by the source corpus.

The neutrino-driven explosion mechanism for core-collapse supernovae in its modern flavor relies on the additional support of hydrodynamical instabilities in achieving shock revival. Two possible candidates, convection and the so-called standing accretion shock instability (SASI), have been proposed for this role. In this paper, we discuss new successful simulations of supernova explosions that shed light on the relative importance of these two instabilities. While convection has so far been observed to grow first in self-consistent hydrodynamical models with multi-group neutrino transport, we here present the first such simulation in which the SASI grows faster while the development of convection is initially inhibited. We illustrate the features of this SASI-dominated regime using an explosion model of a 27 M☉ progenitor, which is contrasted with a convectively dominated model of an 8.1 M☉ progenitor with subsolar metallicity, whose early post-bounce behavior is more in line with previous 11.2 M☉ and 15 M☉ explosion models. We analyze the conditions discriminating between the two different regimes, showing that a high mass-accretion rate and a short advection timescale are conducive for strong SASI activity. We also briefly discuss some important factors for capturing the SASI-driven regime, such as general relativity, the progenitor structure, a nuclear equation of state leading to a compact proto-neutron star, and the neutrino treatment. Finally, we evaluate possible implications of our findings for two-dimensional and three-dimensional supernova simulations.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/84d2034d66932d9583bc31c2200148d143f64add

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Citations in the corpus

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.”
THE ROLE OF TURBULENCE IN NEUTRINO-DRIVEN CORE-COLLAPSE SUPERNOVA EXPLOSIONS (2014, background): “…of multi-dimensional dynamics on the neutrino mechanism (e.g., Burrows et al. 1995; Murphy & Burrows 2008; Marek & Janka 2009; Dolence et al. 2013; Müller et al. 2012b; Bruenn et al. 2013; Takiwaki et al. 2014): multi-dimensional motions increase the dwell time of material in the gain region,…”
THE LANDSCAPE OF THE NEUTRINO MECHANISM OF CORE-COLLAPSE SUPERNOVAE: NEUTRON STAR AND BLACK HOLE MASS FUNCTIONS, EXPLOSION ENERGIES, AND NICKEL YIELDS (2014, methodology): “…progenitors and 2D simulations of different groups using similar physics and performed on the same four progenitors show qualitative differences ranging from full success to complete failure (Müller et al. 2012a; Müller et al., 2013, YITP conference; Bruenn et al. 2013; Dolence et al. 2014).”
A TWO-PARAMETER CRITERION FOR CLASSIFYING THE EXPLODABILITY OF MASSIVE STARS BY THE NEUTRINO-DRIVEN MECHANISM (2015, background): “…one hand, some of the 2D explosions set in relatively late and might remain on the weak side (e.g., Marek & Janka 2009; Suwa 2012; Suwa et al. 2014; Müller et al. 2012a,b, 2013; Müller & Janka 2014), although such apprehension is speculative because not all simulations could be continued until…”
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 ) .”
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).”
The Status of Multi-Dimensional Core-Collapse Supernova Models (2016, background): “…of successful neutrino-driven explosion models has grown from about a handful in mid-2012 (Buras et al. 2006b; Marek & Janka 2009; Suwa et al. 2010; Müller et al. 2012a) to a huge sample of explosion models with ZAMS masses between 10M and 75M , different metallicities, and different choices for…”
A NEW MULTI-DIMENSIONAL GENERAL RELATIVISTIC NEUTRINO HYDRODYNAMICS CODE OF CORE-COLLAPSE SUPERNOVAE. III. GRAVITATIONAL WAVE SIGNALS FROM SUPERNOVA EXPLOSION MODELS (2012, methodology): “For an overview of the current status, the remaining uncertainties of the current generation of models, and future directions in the field the reader should refer to Müller et al. (2012b) as well as recent review articles (Janka 2012; Janka et al. 2012; Kotake et al. 2012; Burrows 2012).”
A COMPARISON OF TWO- AND THREE-DIMENSIONAL NEUTRINO-HYDRODYNAMICS SIMULATIONS OF CORE-COLLAPSE SUPERNOVAE (2013, background): “…state-of-theart two-dimensional (2D) simulations, in which spectral neutrino transport is solved with different levels of sophistication (e.g., Buras et al. (2006); Marek & Janka (2009); Müller et al. (2012, 2013); Bruenn et al. (2013); Suwa et al. (2010, 2011, 2013), Janka (2012) for a review).”
A simple approach to the supernova progenitor–explosion connection (2016, background): “Furthermore, in some multi-D simulations (Marek & Janka 2009 ; M¨uller et al. 2012a; Lentz et al. 2015 ; Melson et al.2015b), shock revival is delayed considerably beyond the infall of the Si/O interface and is instead triggered by a continuing improvement of the heating conditions due to the…”
What can be learned from a future supernova neutrino detection (2017, background): “dominates is seen to be related to the accretion rate [135, 136].”