Simulations of black hole formation and the collapsar scenario - PowerPoint PPT Presentation

Simulations of black hole formation and the collapsar scenario (preliminary) Pablo Cerdá-Durán Nicolas De Brye Miguel Angel Aloy

Numerical setup ● CoCoNuT Code – GR (CFC approximation) – HRSC schemes for hydro – Spectral methods for the metric – Spherical coordinates – Tabulated EOS (LS180 in this talk) – Approximate neutrino treatment (leakage) – Excision inside the apparent horizon – GW: quadrupole formula

BH in CFC (a=0.2)

BH in CFC (a=1.)

Initial models (1D) ● Woosley et al 2002 (20 – 75 M sun ) – “s” : solar metallicity – “u” : low metallicity (10 -4 x solar) – “z” : zero metallicity ● Non-rotating models

1D simulations

1D simulations

1D simulations

1D simulations

Initial models (2D) ● s40 & u40 Woosley et al 2002 ● Equilibrium model with pseudo-barotropic EOS ● Innermost 30000 km ( ~8.3 M sun ) ● 1200x32 grid points (Innermost cell 250 m) ● Rigid rotation – T/W = 0.02 – J/M^2 = 7.2 – r / r equator = 0.75 pole – Central ~ 0.1 rad/s

2D simulations

2D simulations (movies)

2D simulations

Conclusions ● Is BH formation easier than SNe? – Long time to form BH – Instabilities active: SASI/MRI? -> Supernova? – Full neutrino transport + detailed MHD? – BH+SNe? Fallback scenario? ● Can we say something about progenitors? – Collapse mainly determined by inner structure not ZAMS mass?