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

pole / r equator = 0.75

– 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?