3 research outputs found
Erratum: Progenitor-explosion connection and remnant birth masses for neutrino-driven supernovae of iron-core progenitors (2012, ApJ, 757, 69)
An erroneous interpretation of the hydrodynamical results led to an incorrect
determination of the fallback masses in Ugliano et al. (2012), which also (on a
smaller level) affects the neutron star masses provided in that paper. This
problem was already addressed and corrected in the follow-up works by Ertl et
al. (2015) and Sukhbold et al. (2015). Therefore, the reader is advised to use
the new data of the latter two publications. In the remaining text of this
Erratum we present the differences of the old and new fallback results in
detail and explain the origin of the mistake in the original analysis by
Ugliano et al. (2012).Comment: 3 pages, 2 figures; submitted to The Astrophysical Journa
Progenitor-explosion connection and remnant birth masses for neutrino-driven supernovae of iron-core progenitors
We perform hydrodynamic supernova simulations in spherical symmetry for over
100 single stars of solar metallicity to explore the progenitor-explosion and
progenitor-remnant connections established by the neutrino-driven mechanism. We
use an approximative treatment of neutrino transport and replace the
high-density interior of the neutron star (NS) by an inner boundary condition
based on an analytic proto-NS core-cooling model, whose free parameters are
chosen such that explosion energy, nickel production, and energy release by the
compact remnant of progenitors around 20 solar masses are compatible with
Supernova 1987A. Thus we are able to simulate the accretion phase, initiation
of the explosion, subsequent neutrino-driven wind phase for 15-20 s, and the
further evolution of the blast wave for hours to days until fallback is
completed. Our results challenge long-standing paradigms. We find that remnant
mass, launch time, and properties of the explosion depend strongly on the
stellar structure and exhibit large variability even in narrow intervals of the
progenitors' zero-age-main-sequence mass. While all progenitors with masses
below about 15 solar masses yield NSs, black hole (BH) as well as NS formation
is possible for more massive stars, where partial loss of the hydrogen envelope
leads to weak reverse shocks and weak fallback. Our NS baryonic masses of
~1.2-2.0 solar masses and BH masses >6 solar masses are compatible with a
possible lack of low-mass BHs in the empirical distribution. Neutrino heating
accounts for SN energies between some 10^{50} erg and about 2*10^{51} erg, but
can hardly explain more energetic explosions and nickel masses higher than
0.1-0.2 solar masses. These seem to require an alternative SN mechanism.Comment: 10 pages, 6 figures (7 eps files); extended version to account for
referee comments and questions; accepted by Astrophys.
Massive stars and their supernovae
Stars more massive than about 8-10 solar masses evolve differently from their lower-mass counterparts: nuclear energy liberation is possible at higher temperatures and densities, due to gravitational contraction caused by such high masses, until forming an iron core that ends this stellar evolution. The star collapses thereafter, as insufficient pressure support exists when energy release stops due to Fe/Ni possessing the highest nuclear binding per nucleon, and this implosion turns into either a supernova explosion or a compact black hole remnant object. Neutron stars are the likely compact-star remnants after supernova explosions for a certain stellar mass range. In this chapter, we discuss this late-phase evolution of massive stars and their core collapse, including the nuclear reactions and nucleosynthesis products. We also include in this discussion more exotic outcomes, such as magnetic jet supernovae, hypernovae, gamma-ray bursts and neutron star mergers. In all cases we emphasize the viewpoint with respect to the role of radioactivities