Two-dimensional hydrodynamic core-collapse supernova simulations with spectral neutrino transport II. Models for different progenitor stars

By R. Buras, Hans-Thomas Janka, Markus Rampp, K. Kifonidis. 2005

262 citations recorded by the source corpus.

Spherically symmetric (ID) and two-dimensional (2D) supernova simulations for progenitor stars between 11 M ⊙ and 25 M ⊙ are presented, making use of the PROMETHEUS/VERTEX neutrino-hydrodynamics code, which employs a full spectral treatment of neutrino transport and neutrino-matter interactions with a variable Eddington factor closure of the O(v/c) moments equations of neutrino number, energy, and momentum. Multi-dimensional transport aspects are treated by the "ray-by-ray plus" approximation described in Paper I. We discuss in detail the variation of the supernova evolution with the progenitor models, including one calculation for a 15 M ⊙ progenitor whose iron core is assumed to rotate rigidly with an angular frequency of 0.5 rad s -1 before collapse. We also test the sensitivity of our 2D calculations to the angular grid resolution, the lateral wedge size of the computational domain, and to the perturbations which seed convective instabilities in the post-bounce core. In particular, we do not find any important differences depending on whether random perturbations are included already during core collapse or whether such perturbations are imposed on a ID collapse model shortly after core bounce. Convection below the neutrinosphere sets in 30-40 ms after bounce at a density well above 10 12 g cm -3 in all 2D models, and encompasses a layer of growing mass as time goes on. It leads to a more extended proto-neutron star structure with reduced mean energies of the radiated neutrinos, but accelerated lepton number and energy loss and significantly higher muon and tau neutrino luminosities at times later than about 100ms after bounce. While convection inside the nascent neutron star turns out to be insensitive to our variations of the angular cell and grid size, the convective activity in the neutrino-heated postshock layer gains more strength in better resolved models. We find that low (l = 1, 2) convective modes, which require the use of a full 180 degree grid and are excluded in simulations with smaller angular wedges, can qualitatively change the evolution of a model. In case of an 11.2 M ⊙ star, the lowest-mass progenitor we investigate, a probably rather weak explosion by the convectively supported neutrino-heating mechanism develops after about 150ms post-bounce evolution in a 2D simulation with 180 degrees, whereas the same model with 90 degree wedge fails to explode like all other models. This sensitivity demonstrates the proximity of our 2D calculations to the borderline between success and failure, and stresses the need to strive for simulations in 3D, ultimately without the constraints connected with the axis singularity of a polar coordinate grid.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/ff14d3cf4f2fe9acc950f723e2603d30d0e3b86e

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Nuclear and High Energy Physics

Citations in the corpus

Characterizing the Gravitational Wave Signal from Core-collapse Supernovae (2018, background): “…first few hundred milliseconds after core bounce, and/or were obtained from simulations that treated the inner core of the protoneutron star (PNS) in 1D, possibly affecting the development of the inner PNS convection (Buras et al. 2006; Dessart et al. 2006; Radice et al. 2017; Glas et al. 2018).”
REVIVAL OF THE STALLED CORE-COLLAPSE SUPERNOVA SHOCK TRIGGERED BY PRECOLLAPSE ASPHERICITY IN THE PROGENITOR STAR (2013, unknown): “3; Thompson 2000; Janka 2001; Buras et al. 2006; Fernández 2012).”
Exploring Fundamentally Three-dimensional Phenomena in High-fidelity Simulations of Core-collapse Supernovae (2018, background): “This effect, in relation to its impact on the heavy-lepton neutrino luminosities, has been noted in several recent multidimensional studies of CCSNe including O’Connor & Couch (2018); Radice et al. (2017), but note that other multidimensional simulations see a smaller impact Buras et al. (2006).”
THE DEVELOPMENT OF EXPLOSIONS IN AXISYMMETRIC AB INITIO CORE-COLLAPSE SUPERNOVA SIMULATIONS OF 12–25 M ⊙ ?> STARS (2012, methodology): “…with a restricted angular grid (Buras et al. 2003), an explosion commenced at 225 ms after bounce when a full 180-degree angular grid was employed (Buras et al. 2006a), and when continued to 300 ms after bounce reached a diagnostic energy of 0.025 B, increasing at the rate of 1 B s−1 (Marek &…”
GENERAL-RELATIVISTIC SIMULATIONS OF THREE-DIMENSIONAL CORE-COLLAPSE SUPERNOVAE (2012, background): “M solar-metallicity progenitor star of Woosley et al. (2002) obtained with the code and microphysics of Buras et al. (2006b).”
r-Process Nucleosynthesis in Hot Accretion Disk Flows from Black Hole-Neutron Star Mergers (2008, background): “If these conditions were not met, the outflow could have become proton-rich, as can happen in other astrophysical environments (Fröhlich et al. 2006; Buras et al. 2006).”
Features of the Acoustic Mechanism of Core-Collapse Supernova Explosions (2006, methodology): “M⊙ model of WHW02 boasts the thinnest mantle of their whole model set, and this is consistent with the explanation given in §1 for why Buras et al. (2006b) obtained a SASI- and neutrino-aided explosion, albeit weak, but no such explosion for the more massive cores with shallower and thicker density…”
THREE-DIMENSIONAL HYDRODYNAMIC CORE-COLLAPSE SUPERNOVA SIMULATIONS FOR AN 11.2 M☉ STAR WITH SPECTRAL NEUTRINO TRANSPORT (2011, methodology): “These transition timescales are also consistent with Buras et al. (2006) who employed the same progenitor model as ours in their 2D simulations in which detailed neutrino transport was solved (see their Figure 22).”
NEW TWO-DIMENSIONAL MODELS OF SUPERNOVA EXPLOSIONS BY THE NEUTRINO-HEATING MECHANISM: EVIDENCE FOR DIFFERENT INSTABILITY REGIMES IN COLLAPSING STELLAR CORES (2012, methodology): “For our 27M⊙ model, the following differences to other recent two-dimensional first-principle simulations of supernova explosions (Buras et al. 2006a; Marek & Janka 2009; Bruenn et al. 2009; Suwa et al. 2010; Müller et al. 2012) as well as convective models based on a simple light-bulb…”
Two-Dimensional Multiangle, Multigroup Neutrino Radiation-Hydrodynamic Simulations of Postbounce Supernova Cores (2008, methodology): “The multi-D dynamics associated with convective overturn in the postshock region (e.g., Herant et al. 1994; Burrows et al. 1995; Janka & Müller 1996; Buras et al. 2006a) and the recently identified standing accretion shockinstability (SASI, e.g., Foglizzo & Tagger 2000; Foglizzo et al. 2007; Scheck…”
A NEW MULTI-DIMENSIONAL GENERAL RELATIVISTIC NEUTRINO HYDRODYNAMICS CODE FOR CORE-COLLAPSE SUPERNOVAE. II. RELATIVISTIC EXPLOSION MODELS OF CORE-COLLAPSE SUPERNOVAE (2012, methodology): “Both instabilities help to keep the accreted material in the gain region for a longer time before it is advected deeper into the cooling region and onto the neutron star surface (Buras et al. 2006a; Murphy & Burrows 2008).”
Simulations of Magnetically Driven Supernova and Hypernova Explosions in the Context of Rapid Rotation (2007, methodology): “There is an emerging consensus that the core-collapse supernovamechanism is essentially aspherical and that instabilities and the breaking of spherical symmetry are keys to explosion (Buras et al. 2006a, 2006b; Burrows et al. 2006, 2007; Blondin et al. 2003).”
A MODEL FOR GRAVITATIONAL WAVE EMISSION FROM NEUTRINO-DRIVEN CORE-COLLAPSE SUPERNOVAE (2009, background): “…and the SASI, suggest that the neutrino mechanism may yet succeed, though it fails in 1D (Herant et al. 1994; Janka & Müller 1995; Burrows et al. 1995; Janka & Müller 1996; Burrows et al. 2007c; Kitaura et al. 2006; Buras et al. 2006b,a; Marek & Janka 2009; Ott et al. 2008; Murphy & Burrows 2008b).”
Equation-of-state dependent features in shock-oscillation modulated neutrino and gravitational-wave signals from supernovae (2008, methodology): “…used in the present simulations shows a distinct drop in the mass accretion rate by roughly a factor of two when the steep density decline at the interface between the silicon shell and the oxygen-enriched Si layer falls through the stalled shock (see Appendices A and B of Buras et al. 2006b).”
A TWO-PARAMETER CRITERION FOR CLASSIFYING THE EXPLODABILITY OF MASSIVE STARS BY THE NEUTRINO-DRIVEN MECHANISM (2015, background): “This choice of reference density defines a clear standard for the comparison of stellar profiles of different progenitors (cf. Appendix A of Buras et al. 2006).”
BLACK HOLE FORMATION IN FAILING CORE-COLLAPSE SUPERNOVAE (2010, background): “Buras et al. (2006b) who also artificially exploded this progenitor in 1D, though with much more sophisticated neutrino transport, find2 an average heating efficiency of 0.1−0.15 which is consistent with our result.”