Supernova Simulations with Boltzmann Neutrino Transport: A Comparison of Methods

By M. Liebendörfer, Markus Rampp, Hans-Thomas Janka, A. Mezzacappa. 2003

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Accurate neutrino transport has been built into spherically symmetric simulations of stellar core collapse and postbounce evolution. The results of such simulations agree that spherically symmetric models with standard microphysical input fail to explode by the delayed, neutrino-driven mechanism. Independent groups implemented fundamentally different numerical methods to tackle the Boltzmann neutrino transport equation. Here we present a direct and detailed comparison of such neutrino radiation-hydrodynamics simulations for two codes, AGILE-BOLTZTRAN of the Oak Ridge-Basel group and VERTEX of the Garching group. The former solves the Boltzmann equation directly by an implicit, general relativistic discrete-angle method on the adaptive grid of a conservative implicit hydrodynamics code with second-order TVD advection. In contrast, the latter couples a variable Eddington factor technique with an explicit, moving-grid, conservative high-order Riemann solver with important relativistic effects treated by an effective gravitational potential. The presented study is meant to test our neutrino radiation-hydrodynamics implementations and to provide a data basis for comparisons and verifications of supernova codes to be developed in the future. Results are discussed for simulations of the core collapse and postbounce evolution of a 13 M☉ star with Newtonian gravity and a 15 M☉ star with relativistic gravity.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/554b2b710ecfac2871734852250b0d14d4c55be2

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Citations in the corpus

Multidimensional supernova simulations with approximative neutrino transport. II. Convection and the (2007, background): “…energy-dependent description of the neutrino transport (in spherical symmetry see, e.g., Rampp & Janka 2002; Liebendörfer et al. 2001; Liebendörfer et al. 2005; Thompson et al. 2003, and for multi-group transport also in 2D, see, e.g., Buras et al. 2003, 2006a,b) the models presented…”
A NEW MULTI-DIMENSIONAL GENERAL RELATIVISTIC NEUTRINO HYDRODYNAMIC CODE FOR CORE-COLLAPSE SUPERNOVAE. I. METHOD AND CODE TESTS IN SPHERICAL SYMMETRY (2010, methodology): “The treatment of the model Boltzmann equation in CoCoNuT may also be an important factor, either because of the approximations in the tangent-ray scheme (which may affect the transition from the optically thick to the optically thin regime) or because of the superior angular resolution of the tangen”
PREPARING FOR AN EXPLOSION: HYDRODYNAMIC INSTABILITIES AND TURBULENCE IN PRESUPERNOVAE (2013, unknown): “…SN explosions in a self-consistent way (Arnett 1996; Kitaura et al. 2006; Burrows, et al. 2007; Liebendörfer et al. 2001a,b; Rampp, et al. 2002; Buras, et al. 2003; Thompson, Burrows & Pinto 2003; Liebendörfer et al. 2005; Sumiyoshi, et al. 2005; Fryer & Young 2007; Lentz, et al. 2012).”
A MODEL FOR GRAVITATIONAL WAVE EMISSION FROM NEUTRINO-DRIVEN CORE-COLLAPSE SUPERNOVAE (2009, background): “…detailed one-dimensional (1D) simulations have shown that this mechanism, the neutrino mechanism, fails in 1D (Liebendörfer et al. 2001b,a; Rampp & Janka 2002; Buras et al. 2003; Thompson et al. 2003; Liebendörfer et al. 2005), except for the least massive of the massive stars (Kitaura etal.”
Two-Dimensional Multiangle, Multigroup Neutrino Radiation-Hydrodynamic Simulations of Postbounce Supernova Cores (2008, unknown): “While appealing, it has been shown to fail for regular massive stars in spherical symmetry (1D) when the best neutrino physics and transport are used (Rampp & Janka 2000; Liebendörfer et al. 2001; Liebendörfer et al. 2005; Thompson et al. 2003).”
DIMENSION AS A KEY TO THE NEUTRINO MECHANISM OF CORE-COLLAPSE SUPERNOVA EXPLOSIONS (2010, methodology): “The Liebendörfer et al. (2005) scheme for determining the electron fraction on infall was used, which involves tying Ye to the mass density achieved for densities below the trapping density.”
Nucleosynthesis-relevant conditions in neutrino-driven supernova outflows. I. Spherically symmetric (2006, background): “Liebendörfer et al. (2005) compared the dynamics and neutrino emission during the collapse phase, core bounce, and early post-bounce evolution in 1D (see also Marek et al. 2006).”
Protoneutron star evolution and the neutrino-driven wind in general relativistic neutrino radiation hydrodynamics simulations (2009, background): “(8) in Liebendörfer et al. (2005)) and due to neutrino-matter interactions such as emission and absorption as well as scattering and pair reactions.”
The Status of Multi-Dimensional Core-Collapse Supernova Models (2016, methodology): “…general relativistic effects have demonstrated that the neutrino-driven mechanism is not viable in spherical symmetry (Rampp & Janka 2000, 2002; Liebendörfer et al. 2001, 2004, 2005; Sumiyoshi et al. 2005; Buras et al. 2006a,b; Müller et al. 2010; Fischer et al. 2010; Lentz et al. 2012a,b),…”
Supernova Nucleosynthesis in Population III 13-50 M☉ Stars and Abundance Patterns of Extremely Metal-poor Stars (2007, result): “How- ever, recent studies (e.g., Rampp & Janka 2000; Liebendörfer et al. 2005; Fröhlich et al. 2006b; Buras et al. 2006a, 2006b) have suggested that Ye may be significantly varied by the neutrino process during explosion.”