A full general relativistic neutrino radiation-hydrodynamics simulation of a collapsing very massive star and the formation of a black hole

Abstract

We study the final fate of a very massive star by performing full general relativistic (GR), three-dimensional (3D) simulation with three-flavor multi-energy neutrino transport. Utilizing a 70 solar mass zero metallicity progenitor, we self-consistently follow the radiation-hydrodynamics from the onset of gravitational core-collapse until the second collapse of the proto-neutron star (PNS), leading to black hole (BH) formation. Our results show that the BH formation occurs at a post-bounce time of T pb ∼ 300 ms for the 70 M ⊙ star. This is significantly earlier than those in the literature where lower mass progenitors were employed. At a few ∼ 10 ms before BH formation, we find that the stalled bounce shock is revived by intense neutrino heating from the very hot PNS, which is aided by violent convection behind the shock. In the context of 3D-GR core-collapse modeling with multi-energy neutrino transport, our numerical results present the first evidence to validate a fallback BH formation scenario of the 70M ⊙ star.

Three-dimensional core-collapse supernova simulations of massive and rotating progenitors

“…Simulating CCSNe with larger progenitor masses will also enable us to further study the relationship between compactness and explodability found in previous studies (O'Connor & Ott 2011). Intriguingly and in contrast to O'Connor & Ott (2011), a number of 3D neutrino-driven simulations (Chan et al 2018;Ott et al 2018;Kuroda et al 2018;Burrows et al 2020Burrows et al , 2019Walk et al 2019) observed shock expansion in some progenitors with rather massive and compact cores. From the point of view of gravitational-wave astronomy, high-mass progenitors are particularly interesting because they are expected to explode more energetically (Müller et al 2016a), which will result in stronger gravitational-wave emission (Müller 2017;Powell & Müller 2019;Radice et al 2019).…”

Sensitivity of the lower edge of the pair-instability black hole mass gap to the treatment of time-dependent convection

“…Our main parameter of interest is the resulting BH mass, which we estimate using the mass coordinate where the gravitational binding energy reaches 10 48 ergs. This allows for the possibility of mass loss during the final corecollapse from either a weak explosion (Ott et al 2018;Kuroda et al 2018), energy loss to neutrinos, or ejection of a fraction of the envelope caused by the latter (e.g., Nadezhin 1980;Lovegrove & Woosley 2013). This typically gives estimated BH masses within a few 0.01 M of the total baryonic mass slower than the escape velocity at the onset of core collapse.…”

Features of Accretion-phase Gravitational-wave Emission from Two-dimensional Rotating Core-collapse Supernovae

“…Morozova et al (2018) investigate GW emission for moderate rotational speeds (Ω core = 0.2 rad s −1 ) for a single progenitor mass (13M ) over 1 second postbounce. Pan et al (2018), Kuroda et al (2018), Cerdá-Durán et al (2013), and Ott et al (2011) investigate the relationship between black hole formation and GW emission, for a nonrotating 40 M , a nonrotating 70 M , a rotating 35 M , and a rotating 75 M progenitor, respectively. These studies also find stronger GW emission at bounce with increased progenitor angular momentum and loud GW emission at later times for nonrotating CCSNe.…”