Shock Breakout in Core-Collapse Supernovae and Its Neutrino Signature

By T. Thompson, Adam Burrows, P. Pinto. 2002

319 citations recorded by the source corpus.

We present results from dynamical models of core-collapse supernovae in one spatial dimension, employing a newly developed Boltzmann neutrino radiation transport algorithm, coupled to Newtonian Lagrangian hydrodynamics and a consistent high-density nuclear equation of state. The transport method is multigroup, employs the Feautrier technique, uses the tangent-ray approach to resolve angles, is implicit in time, and is second-order accurate in space. We focus on shock breakout and follow the dynamical evolution of the cores of 11, 15, and 20 M☉ progenitors through collapse and the first 250 ms after bounce. The shock breakout burst is the signal event in core-collapse evolution, is the brightest phenomenon in astrophysics, and is largely responsible for the initial debilitation and stagnation of the bounce shock. As such, its detection and characterization could test fundamental aspects of the current collapse/supernova paradigm. We examine the effects on the emergent neutrino spectra, light curves, and mix of species (particularly in the early postbounce epoch) of artificial opacity changes, the number of energy groups, the weak magnetism/recoil corrections, nucleon-nucleon bremsstrahlung, neutrino-electron scattering, and the compressibility of nuclear matter. Furthermore, we present the first high-resolution look at the angular distribution of the neutrino radiation field both in the semitransparent regime and at large radii and explore the accuracy with which our tangent-ray method tracks the free propagation of a pulse of radiation in a near vacuum. Finally, we fold the emergent neutrino spectra with the efficiencies and detection processes for a selection of modern underground neutrino observatories and argue that the prompt electron-neutrino breakout burst from the next galactic supernova is in principle observable and usefully diagnostic of fundamental collapse/supernova behavior. Although we are not in this study focusing on the supernova mechanism per se, our simulations support the theoretical conclusion (already reached by others) that spherical (one-dimensional) supernovae do not explode when good physics and transport methods are employed.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/65ae48cd3a1fdcda5a1b9d9704d8e01869263ea2

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Citations in the corpus

Multidimensional Simulations of the Accretion-induced Collapse of White Dwarfs to Neutron Stars (2006, result): “Note that this definition 15 of the neutrino “average” energy is similar to that found in Thompson et al. (2003), who used the mean intensity Jν in place of the flux Fν .”
THE ROLE OF TURBULENCE IN NEUTRINO-DRIVEN CORE-COLLAPSE SUPERNOVA EXPLOSIONS (2014, background): “Detailed spherically-symmetric (1D) simulations have shown that the neutrino mechanism generally fails to produce explosions (e.g., Liebendörfer et al. 2003; Thompson et al. 2003; Rampp & Janka 2000) for all but the lowest-mass progenitors (Kitaura et al. 2006).”
A Finite Difference Representation of Neutrino Radiation Hydrodynamics in Spherically Symmetric General Relativistic Spacetime (2002, methodology): “It has been assigned to a decrease in the free proton fraction when the shock is formed (Thompson et al. 2003).”
Multidimensional supernova simulations with approximative neutrino transport. I. Neutron star kicks and the anisotropy of neutrino-driven explosions in two spatial dimensions (2006, background): “4−6, and compare with Liebendörfer et al. 2001; Liebendörfer et al. 2005; Rampp & Janka 2000; Buras et al. 2003, 2006a,b; and Thompson et al. 2003).”
IceCube sensitivity for low-energy neutrinos from nearby supernovae (2011, background): “According to Thompson et al. (2003) and Buras et al. (2003), the mean energy is expected to be about (13 – 14) MeV forνe, (14 – 16) MeV forν̄e and (20 – 21) MeV for all other flavors (νx); the Garching model (Kitaura et al., 2006) differs in that the mean energies for ¯νe andνx turn out to be…”
Two-Dimensional Multiangle, Multigroup Neutrino Radiation-Hydrodynamic Simulations of Postbounce Supernova Cores (2008, methodology): “%) relevance for the trapped electron fraction (Ye) and entropy of the inner core at core bounce, but otherwise arguably quite subdominant (Thompson et al. 2003).”
BLACK HOLE FORMATION IN FAILING CORE-COLLAPSE SUPERNOVAE (2010, methodology): “In agreement with previous work that employed a more accurate neutrino treatment (e.g., Thompson et al. 2003; Liebendörfer et al. 2005), the 1D neutrino mechanism is manifestly ineffective in driving the shock, yielding, in this model, a heating efficiency η = Labsorbed/Lνe+ν̄e of only ∼ 3% (on…”
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…”
Viscosity and Rotation in Core-Collapse Supernovae (2004, methodology): “…recent one-dimensional models are fully spectral and multiangle (Rampp & Janka 2000, 2002; Liebendörfer et al. 2001a, 2001b; Mezzacappa et al. 2001; Thompson et al. 2003); neutrino transport also presents the most significant technical hurdle in calculating realistic models of core collapse in…”
The overarching framework of core-collapse supernova explosions as revealed by 3D fornax simulations (2019, methodology): “Inelastic scattering of neutrinos and anti-neutrinos off electrons and free nucleons is addressed using the prescriptions described in Thompson et al. (2003), with more details of its implementation to be found in Burrows & Thompson (2004).”
CORE-COLLAPSE SUPERNOVA EXPLOSIONS TRIGGERED BY A QUARK–HADRON PHASE TRANSITION DURING THE EARLY POST-BOUNCE PHASE (2010, background): “For these progenitors, spherically symmetric simulations do not result in explosions via the delayed neutrino heating mechanism (see e.g. Rampp & Janka 2000; Liebendörfer et al. 2001b; Janka 2001; Thompson et al. 2003).”
Gravitational Waves from Axisymmetric, Rotating Stellar Core Collapse (2003, methodology): “…weak-interaction physics and neutrino transport indicate that the bounce shock does indeed initially stall (Rampp & Janka 2002; Liebendörfer et al. 2001a, 2001b; Thompson et al. 2003), the distinctive character of the s20 model may in fact be more generic than that of our s11 and s15 models.”
Supernova Simulations with Boltzmann Neutrino Transport: A Comparison of Methods (2003, methodology): “…feasible to provide solutions to the Boltzmann transport equation not only for the collapse phase (Mezzacappa & Bruenn 1993b) but also in consistent dynamical simulations of the postbounce evolution (Rampp & Janka 2000; Mezzacappa et al. 2001; Liebendörfer et al. 2001b; Thompson et al. 2003).”
AN OPEN-SOURCE NEUTRINO RADIATION HYDRODYNAMICS CODE FOR CORE-COLLAPSE SUPERNOVAE (2014, methodology): “One can also define moment schemes where the closure is not analytic, but rather one has 3 a variable Eddington tensor (Burrows et al. 2000; Thompson et al. 2003; Rampp & Janka 2002; Buras et al. 2006b,a).”