CCoorere-c-coollallappssee ssuuppeernrnoovvaaee andand gravitationalgravitational waveswaves Christian Y. Cardall Oak Ridge National Laboratory Physics Division University of Tennessee, Knoxville Department of Physics and Astronomy Terascale Supernova Initiative http://www.phy.utk.edu/tsi WWhahatt aarere ccoreore-c-collaollapspsee supernovae?supernovae? SSuurrvveeyy ooff ccoollallappssee ssimimuulalatiotionnss SomSomee gravitationalgravitational wavewave pphheennoommeennoolologgyy Core-collapse supernovae and gravitational waves Christian Y. Cardall TAUP2003, University of Washington, Seattle, 5-9 September 2003 WWhahatt aarere ccoreore-c-collaollapspsee supernovae?supernovae? Core-collapse supernovae and gravitational waves Christian Y. Cardall TAUP2003, University of Washington, Seattle, 5-9 September 2003 SN 1998aq (in NGC 3982) Core-collapse supernovae and gravitational waves Christian Y. Cardall TAUP2003, University of Washington, Seattle, 5-9 September 2003 Spectral classification of supernovae: Type I: Absence of H; Type Ia: Strong Si feature; Type Ib: Absent or weak Si features, strong He; Type Ic: Absent or weak Si features, absent or weak He. Type II: Obvious H features; Type IIL, IIP: Absorption features; Type IIn: Absent or weak absorption features, prominent and narrow H emission. Core-collapse supernovae and gravitational waves Christian Y. Cardall TAUP2003, University of Washington, Seattle, 5-9 September 2003 Physical classification of supernovae: Thermonuclear runaway; Type Ia, accretion onto a white dwarf. Core-collapse supernovae and gravitational waves Christian Y. Cardall TAUP2003, University of Washington, Seattle, 5-9 September 2003 Physical classification of supernovae: Core collapse of a massive star; Type II, outer H layer remains at collapse; Type Ib, outer H layer stripped before collapse; Type Ic, outer H and He layers stripped before collapse. Core-collapse supernovae and gravitational waves Christian Y. Cardall TAUP2003, University of Washington, Seattle, 5-9 September 2003 Does spherical symmetry bring tears to your eyes? Realistic progenitors… Rotation Magnetic fields …will give rise to aspherical collapse. A lot of mass going to high density High infall velocities After core bounce, more asphericity: Triaxial instabilities Anisotropic neutrino emission Convection Accretion shock instability R-mode instability (longer time scales) Core-collapse supernovae and gravitational waves Christian Y. Cardall TAUP2003, University of Washington, Seattle, 5-9 September 2003 Core-collapse supernovae and gravitational waves Christian Y. Cardall TAUP2003, University of Washington, Seattle, 5-9 September 2003 The observables to understand include Explosion; Neutrinos; Pulsar spins, kick velocities, and magnetic fields; Gravitational waves; Element abundances; Measurements across the EM spectrum, IR, optical, UV, X-ray, gamma-ray; images, light curves, spectra, polarimetry... Core-collapse supernovae and gravitational waves Christian Y. Cardall TAUP2003, University of Washington, Seattle, 5-9 September 2003 SSuurrvveeyy ooff ccoollallappssee ssimimuulalatiotionnss Core-collapse supernovae and gravitational waves Christian Y. Cardall TAUP2003, University of Washington, Seattle, 5-9 September 2003 Some key pieces of physics are Neutrino transport/interactions, Spatial dimensionality; Dependence on energy and angles; Relativity; Comprehensiveness of interactions; (Magneto)Hydrodynamics/gravitation, Dimensionality; Relativity; Equation of state/composition, Dense matter treatments; Number and evolution of nuclear species; Diagnostics, Accounting of lepton number; Accounting of total energy. Core-collapse supernovae and gravitational waves Christian Y. Cardall TAUP2003, University of Washington, Seattle, 5-9 September 2003 Simulations of collapse and explosion Multiple spatial dimensions, simplified neutrino transport Fryer & Warren (2002) Burrows, Hayes, & Fryxell (1995) Core-collapse supernovae and gravitational waves Christian Y. Cardall TAUP2003, University of Washington, Seattle, 5-9 September 2003 Simulations of collapse and explosion Multiple spatial dimensions, simplified neutrino transport Janka & Mueller (1996) Mezzacappa, Calder, Bruenn, Blondin, Guidry, Strayer, & Umar (1998) Core-collapse supernovae and gravitational waves Christian Y. Cardall TAUP2003, University of Washington, Seattle, 5-9 September 2003 Simulations of collapse and explosion Spherical symmetry, sophisticated neutrino transport Rampp & Janka (2000) Core-collapse supernovae and gravitational waves Christian Y. Cardall TAUP2003, University of Washington, Seattle, 5-9 September 2003 Simulations of collapse and explosion Spherical symmetry, sophisticated neutrino transport Liebendoerfer, Mezzacappa, Thielemann, Messer, Hix, & Bruenn (2001) Core-collapse supernovae and gravitational waves Christian Y. Cardall TAUP2003, University of Washington, Seattle, 5-9 September 2003 Simulations of collapse and explosion Spherical symmetry, sophisticated neutrino transport Thompson, Burrows, & Pinto (2002) Core-collapse supernovae and gravitational waves Christian Y. Cardall TAUP2003, University of Washington, Seattle, 5-9 September 2003 Simulations of collapse and explosion Multiple spatial dimensions, intermediate neutrino transport Janka, Buras, & Rampp (2002) Core-collapse supernovae and gravitational waves Christian Y. Cardall TAUP2003, University of Washington, Seattle, 5-9 September 2003 SomSomee gravitationalgravitational wavewave pphheennoommeennoolologgyy Core-collapse supernovae and gravitational waves Christian Y. Cardall TAUP2003, University of Washington, Seattle, 5-9 September 2003 Collapse and bounce “Improvements” in Ott, Burrows, Livne, and Rolf, astro-ph/0307472 “Realistic” finite temperature nuclear equation of state Progenitors that include prescriptions for angular momentum transport, mass loss, and magnetic fields These tend to give more pessimistic results Absent in Ott et al. No neutrino transport (shock does not stall in most models) Only two spatial dimensions (no triaxial instabilities) Newtonian gravity (relativity affects infall and maximum densities; post-processing via quadrupole formalism Core-collapse supernovae and gravitational waves Christian Y. Cardall TAUP2003, University of Washington, Seattle, 5-9 September 2003 Collapse and bounce Effects of increasing progenitor core rotation Core-collapse supernovae and gravitational waves Christian Y. Cardall TAUP2003, University of Washington, Seattle, 5-9 September 2003 Collapse and bounce Effects of increasing progenitor core mass Core-collapse supernovae and gravitational waves Christian Y. Cardall TAUP2003, University of Washington, Seattle, 5-9 September 2003 Core-collapse supernovae and gravitational waves Christian Y. Cardall TAUP2003, University of Washington, Seattle, 5-9 September 2003 Accretion shock instability A standing accretion shock, an analytic solution in spherical symmetry, is used as an initial condition. Blondin, Mezzacappa, & DeMarino (2003) Core-collapse supernovae and gravitational waves Christian Y. Cardall TAUP2003, University of Washington, Seattle, 5-9 September 2003 Accretion shock instability The standing accretion shock is unstable in 2D/3D to the point of explosion. Core-collapse supernovae and gravitational waves Christian Y. Cardall TAUP2003, University of Washington, Seattle, 5-9 September 2003 Core-collapse supernovae and gravitational waves Christian Y. Cardall TAUP2003, University of Washington, Seattle, 5-9 September 2003 Core-collapse supernovae and gravitational waves Christian Y. Cardall TAUP2003, University of Washington, Seattle, 5-9 September 2003 Brown, Blondin , and Mezzacappa (2003) -13 EGW ª 3 ¥10 M Core-collapse supernovae and gravitational waves Christian Y. Cardall TAUP2003, University of Washington, Seattle, 5-9 September 2003 SAS Core-collapse supernovae and gravitational waves Christian Y. Cardall TAUP2003, University of Washington, Seattle, 5-9 September 2003 CCoonncclulussioionnss Core-collapse supernovae are dramatic events with a rich phenomenology, including gravitational radiation. Gravitational radiation will be principally correlated with neutrino emission and neutron star kicks. Simulations in multiple spatial dimensions and energy- and angle-dependent neutrino transport are in their infancy. Core collapse and bounce in a galactic supernova may be visible by first-generation LIGO, but detailed understanding awaits next-generation progenitors and simulations. Core-collapse supernovae and gravitational waves Christian Y. Cardall TAUP2003, University of Washington, Seattle, 5-9 September 2003.