Features of the Acoustic Mechanism of Core-Collapse Supernova Explosions

By Adam Burrows, E. Livne, L. Dessart, Christian D. Ott, J. Murphy. 2006

172 citations recorded by the source corpus.

In the context of 2D, axisymmetric, multigroup, radiation/hydrodynamic simulations of core-collapse supernovae over the full 180° domain, we present an exploration of the progenitor dependence of the acoustic mechanism of explosion. All progenitor models we have tested with our Newtonian code explode. However, some of the cores left behind in our simulations, particularly for the more massive progenitors, have baryon masses that are larger than the canonical ~1.5 M☉ of well-measured pulsars. We investigate the roles of the standing accretion shock instability (SASI), the excitation of core g-modes, the generation of core acoustic power, the ejection of matter with r-process potential, the windlike character of the explosion, and the fundamental anisotropy of the blasts. We find that the breaking of spherical symmetry is central to the supernova phenomenon, the delays to explosion can be long, and the blasts, when top-bottom asymmetric, are self-collimating. We see indications that the initial explosion energies are larger for the more massive progenitors and smaller for the less massive progenitors and that the neutrino contribution to the explosion energy may be an increasing function of progenitor mass. However, the explosion energy is still accumulating by the end of our simulations and has not converged to final values. The degree of explosion asymmetry we obtain is completely consistent with that inferred from the polarization measurements of Type Ic supernovae. Furthermore, we calculate for the first time the magnitude and sign of the net impulse on the core due to anisotropic neutrino emission and suggest that hydrodynamic and neutrino recoils in the context of our asymmetric explosions afford a natural mechanism for observed pulsar proper motions.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/7f6e25e6e6430f46865309bf50a9d0c2af0e61b7

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Citations in the corpus

THREE-DIMENSIONAL HYDRODYNAMIC CORE-COLLAPSE SUPERNOVA SIMULATIONS FOR AN 11.2 M☉ STAR WITH SPECTRAL NEUTRINO TRANSPORT (2011, background): “The dependence of progenitors (e.g., Buras et al. (2006); Burrows et al. (2007b)) and equations of state (e.g., Marek & Janka (2009)) are important to be clarified in 3D computations.”
AN OPEN-SOURCE NEUTRINO RADIATION HYDRODYNAMICS CODE FOR CORE-COLLAPSE SUPERNOVAE (2014, background): “Examples in the CCSN context include Bruenn (1985) in 1D and Fryer (1999); Burrows et al. (2007); Swesty & Myra (2009); Yakunin et al. (2010); Zhang et al. (2013) in 2D.”
IS STRONG SASI ACTIVITY THE KEY TO SUCCESSFUL NEUTRINO-DRIVEN SUPERNOVA EXPLOSIONS? (2011, background): “…for a wider range of progenitors (Bruenn et al. 2009), while in purely Newtonian simulations with multi-dimensional neutrino diffusion (including energy dependence but without energy-bin coupling) Burrows et al. (2006, 2007) could not see any success of the delayed neutrino-driven mechanism.”
COMPACT REMNANT MASS FUNCTION: DEPENDENCE ON THE EXPLOSION MECHANISM AND METALLICITY (2011, background): “One model allows for considerable contribution from the SASI engine, a current focus of many supernova groups (Blondin (A color version of this figure is available in the online journal.) et al. 2003; Burrows et al. 2007; Bruenn et al. 2009; Scheck et al. 2008; Marek & Janka 2009).”
NEW EQUATIONS OF STATE IN SIMULATIONS OF CORE-COLLAPSE SUPERNOVAE (2011, background): “These models have shown to increase the neutrino heating efficiency (see, e.g., Miller et al. (1993), Herant et al. (1994), Janka & Mueller (1996), Burrows et al. (2007)) and help to aid the understanding of aspherical explosions (see, for example, Bruenn et al. (2006); Marek & Janka (2009); and…”
Core-collapse explosions of Wolf–Rayet stars and the connection to Type IIb/Ib/Ic supernovae (2011, background): “A second issue is the viability of the explosion mechanism for stars of increasing mass, since their higher-mass cores are increasingly more bound,exposing the newly-formed SN shock to a tremendous accretion rate (Burrows et al. 2007).”
Multiple physical elements to determine the gravitational-wave signatures of core-collapse supernovae (2011, methodology): “If the core pulsation energy given in Burrows et al. (2007) [78] could be used to measure the explosion energy in the acoustic mechanism, they reach to 1 B after 1000ms after bounce11.”
Criteria for Core-Collapse Supernova Explosions by the Neutrino Mechanism (2008, methodology): “Furthermore Burrows et al. (2006), Burrows et al. (2007d), Burrows et al. (2007c), Burrows et al. (2007a), and Burrows et al. (2007b), using VULCAN/2D (Livne 1993; Livne et al. 2004) and multi-group flux-limited diffusion (MGFLD), obtain successful explosions only for the 8.8-”
Nebular emission-line profiles of Type Ib/c supernovae - Probing the ejecta asphericity (2009, background): “Strong neutron star kicks (up to several hundred km s−1 ) have indeed been observed (e.g. Cordes, Romani & Lundgren 1993) and reproduced in simulations of anisotropic explosions with dominant dipole (l = 1) mode in the ejecta (Burrows & Hayes 1996; Scheck et al. 2004, 2006; Burrows et al. 2007).”
Two-Dimensional Multiangle, Multigroup Neutrino Radiation-Hydrodynamic Simulations of Postbounce Supernova Cores (2008, methodology): “The module implementing 2D transport in the MGFLD approximation, evolving the zeroth moment of the radiation field, is discussed in Burrows et al. (2007c).”
A MODEL FOR GRAVITATIONAL WAVE EMISSION FROM NEUTRINO-DRIVEN CORE-COLLAPSE SUPERNOVAE (2009, methodology): “…mechanism (Marek & Janka 2009; Murphy & Burrows 2008b), the acoustic mechanism (Burrows et al. 2006, 2007c), or magnetohydrodynamic (MHD) jets (Burrows et al. 2007b; Dessart et al. 2008 and references therein), viable explosion mechanisms for all but the least massive of massive stars…”
DIMENSION AS A KEY TO THE NEUTRINO MECHANISM OF CORE-COLLAPSE SUPERNOVA EXPLOSIONS (2010, methodology): “Two-dimensional models also enable accretion in one quadrant to power explosion in another (Burrows et al. 2007b), something impossible in 1D and one reason neutrino-driven explosions in 1D are generally thwarted.”
The Status of Multi-Dimensional Core-Collapse Supernova Models (2016, methodology): “Using modern multi-group neutrino transport, this was demonstrated by Kitaura et al. (2006) for the progenitor of Nomoto (1984, 1987) and confirmed in subsequent simulations by different groups (Janka et al. 2008; Burrows et al. 2007b; Fischer et al. 2010).”
A successful 3D core-collapse supernova explosion model (2018, background): “By the end of the simulation, an exploding debris field is accompanied by simultaneous inward accretion between the expanding lobes of some of the inner-progenitor matter, partly responsible for maintaining a driving neutrino luminosity (Burrows et al. 2007a).”
DELAYED NEUTRINO-DRIVEN SUPERNOVA EXPLOSIONS AIDED BY THE STANDING ACCRETION-SHOCK INSTABILITY (2007, background): “Burrows et al. (2006, 2007b) estimated that the acoustic energy flux generated by this gravity-wave activity of the forming compact remnant dominates the energy deposition by neutrinos in their models at times later than about one second after bounce.”