Probing the gravitational well: no supernova explosion in spherical symmetry with general relativistic boltzmann neutrino transport

By M. Liebendoerfer, A. Mezzacappa, F. Thielemann, O. E. Bronson Messer, W. Hix, S. W. B. U. O. Basel, Oak Ridge National Laboratory, U. Tennessee, J. S. F. D. S. Research, Florida Atlantic University. 2000

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We report on the stellar core collapse, bounce, and postbounce evolution of a 13 M{sub 0} star in a self-consistent general relativistic spherically symmetric simulation based on Boltzmann neutrino transport. We conclude that approximations to exact neutrino transport and the omission of general relativistic effects were not alone responsible for the failure of numerous preceding attempts to model supernova explosions in spherical symmetry. Compared to simulations in Newtonian gravity, the general relativistic simulation results in a smaller shock radius. We however argue that the higher neutrino luminosities and rms energies in the general relativistic case could lead to a larger supernova explosion energy.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/fe69d381a08007f5cb26c9c53d1ea28c6b03b2ff

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Citations in the corpus

Neutrino-dominated Accretion and Supernovae (2005, background): “…different groups with improved neutrino transport and fully relativistic hydrodynamics (Bruenn 1985; Bruenn & Mezzacappa 1997; Bruenn et al. 2001; Liebendorfer et al. 2001, 2005; Mezzacappa et al. 2001; Myra & Burrows 1990; Rampp & Janka 2000; Thompson et al. 2003), have demonstrated…”
Protoneutron star evolution and the neutrino-driven wind in general relativistic neutrino radiation hydrodynamics simulations (2009, background): “…= Γe + 2 Γ + 1 ( u2 2 − m r ) , (8) which in turn is the sum of the specific internal energy e 1, the specific kinetic energy given by the fluid velocity u = ∂r/α∂t squared and the specific gravitational binding energy m/r with gravitational mass m and radius r (see Liebendörfer et al. (2001b)).”
Monte Carlo Study of Supernova Neutrino Spectra Formation (2002, methodology): “Finally, we include two simulations similar to the Accretion-Phase Model I, one by Mezzacappa et al. (2001) and the other by Liebendörfer et al. (2001).”
Multidimensional supernova simulations with approximative neutrino transport. II. Convection and the (2007, methodology): “…simulations with a state-of-the-art 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,…”
Colloquium: Perspectives on core-collapse supernova theory (2012, background): “…core collapse, but the papers by Arnett (1966,1967,1977), Imshennik & Nadëzhin (1973), Bowers & Wilson (1982), Bruenn (1985), Mayle & Wilson (1988), Liebendörfer et al. (2001), Liebendörfer, Rampp, Janka, & Mezzacappa (2005), Burrows et al. (2000), Livne et al. (2004,2007), and Swesty & Myra…”
Composition of the Innermost Core-Collapse Supernova Ejecta (2004, background): “…with accurate neutrino transport have even exceeded the estimates, consistently finding values of Ye > 0.5 in the vicinity of the mass cut in explosion settings (Liebendörfer et al. 2001; Buras et al. 2003; Janka et al. 2003; Thompson et al. 2004; Pruet et al. 2005; Fröhlich et al. 2005a).”
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).”
Shock Breakout in Core-Collapse Supernovae and Its Neutrino Signature (2002, methodology): “Both Liebendörfer et al. (2001) and Rampp & Janka (2000) obtainLpeakνe of ∼ 3.5×10 53 erg s−1 with comparable progenitors.”
The Status of Multi-Dimensional Core-Collapse Supernova Models (2016, methodology): “1D simulations of the post-bounce phase using Boltzmann solvers for the neutrino transport convincingly demonstrated that neutrino-driven explosions cannot be obtained under such conditions in spherical symmetry (Liebendörfer et al. 2001; Rampp & Janka 2000; Burrows et al. 2000a).”
THE DEVELOPMENT OF EXPLOSIONS IN AXISYMMETRIC AB INITIO CORE-COLLAPSE SUPERNOVA SIMULATIONS OF 12–25 M ⊙ ?> STARS (2012, methodology): “…forty years after Colgate and White’s original proposal, with simulations that implemented general relativistic Boltzmann neutrino transport and hydrodynamics coupled to general relativistic gravity, using state of the art weakinteractions and equations of state (Liebendörfer et al. 2001, 2004).”
CORE-COLLAPSE SUPERNOVA EXPLOSIONS TRIGGERED BY A QUARK–HADRON PHASE TRANSITION DURING THE EARLY POST-BOUNCE PHASE (2010, methodology): “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).”
A NEW CLASS OF LUMINOUS TRANSIENTS AND A FIRST CENSUS OF THEIR MASSIVE STELLAR PROGENITORS (2008, background): “The physical mechanism of iron core-collapse supernovae is unknown (Rampp & Janka 2000; Liebendörfer et al. 2001; Thompson et al. 2003; Buras et al. 2003; Burrows et al. 2006).”
NEW EQUATIONS OF STATE IN SIMULATIONS OF CORE-COLLAPSE SUPERNOVAE (2011, methodology): “It was extended to solve the general relativistic equations for both hydrodynamics and neutrino transport in Liebendörfer et al. (2001), based on the following line-element ds2 = α2dt2 + ( r′ Γ )2 da2 + r2dΩ in co-moving coordinates system time t and enclosed baryon mass a, with metric…”
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).”
Features of the Acoustic Mechanism of Core-Collapse Supernova Explosions (2006, background): “…stalled bounce shock is reenergized by neutrino energy deposition after a slight delay, perhaps aided by overturning instabilities in this “gain region,” has been the working hypothesis of the community for the last twenty years (Bethe & Wilson 1985; Buras et al. 2006ab; Liebendörfer et al. 2001).”
THE ISOTROPIC DIFFUSION SOURCE APPROXIMATION FOR SUPERNOVA NEUTRINO TRANSPORT (2007, background): “In the mean time, the spherically symmetric Boltzmann transport equation is routinely solved for all neutrino flavours in dynamical models of stellar core collapse and postbounce evolution (Liebendörfer et al. 2001; Rampp & Janka 2002; Thompson et al. 2003; Sumiyoshi et al. 2005).”