We have simulated the collapse and evolution of the core of a solar-metallicity 40
The hadron-quark phase transition in quantum chromodynamics has been suggested as an alternative explosion mechanism for core-collapse supernovae. We study the impact of three different hadron-quark equations of state (EoS) with first-order (DD2F_SF, STOS-B145) and second-order (CMF) phase transitions on supernova dynamics by performing 97 simulations for solar- and zero-metallicity progenitors in the range of $14\tt {-}100\, \text{M}_\odot$. We find explosions only for two low-compactness models (14 and $16\, \text{M}_\odot$) with the DD2F_SF EoS, both with low explosion energies of ${\sim }10^{50}\, \mathrm{erg}$. These weak explosions are characterized by a neutrino signal with several minibursts in the explosion phase due to complex reverse shock dynamics, in addition to the typical second neutrino burst for phase-transition-driven explosions. The nucleosynthesis shows significant overproduction of nuclei such as 90Zr for the $14\hbox{-} \text{M}_\odot$ zero-metallicity model and 94Zr for the $16\hbox{-}\text{M}_\odot$ solar-metallicity model, but the overproduction factors are not large enough to place constraints on the occurrence of such explosions. Several other low-compactness models using the DD2F_SF EoS and two high-compactness models using the STOS EoS end up as failed explosions and emit a second neutrino burst. For the CMF EoS, the phase transition never leads to a second bounce and explosion. For all three EoS, inverted convection occurs deep in the core of the protocompact star due to anomalous behaviour of thermodynamic derivatives in the mixed phase, which heats the core to entropies up to 4kB/baryon and may have a distinctive gravitational-wave signature, also for a second-order phase transition.
more » « less- NSF-PAR ID:
- 10371473
- Publisher / Repository:
- Oxford University Press
- Date Published:
- Journal Name:
- Monthly Notices of the Royal Astronomical Society
- Volume:
- 516
- Issue:
- 2
- ISSN:
- 0035-8711
- Page Range / eLocation ID:
- p. 2554-2574
- Format(s):
- Medium: X
- Sponsoring Org:
- National Science Foundation
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Abstract M ⊙star and find that it explodes vigorously by the neutrino mechanism, despite its very high “compactness.” Within ∼1.5 s of explosion, a black hole forms. The explosion is very asymmetrical and has a total explosion energy of ∼1.6 × 1051erg. At black hole formation, its baryon mass is ∼2.434M ⊙and gravitational mass is 2.286M ⊙. Seven seconds after black hole formation, an additional ∼0.2M ⊙is accreted, leaving a black hole baryon mass of ∼2.63M ⊙. A disk forms around the proto−neutron star, from which a pair of neutrino-driven jets emanates. These jets accelerate some of the matter up to speeds of ∼45,000 km s−1and contain matter with entropies of ∼50. The large spatial asymmetry in the explosion results in a residual black hole recoil speed of ∼1000 km s−1. This novel black hole formation channel now joins the other black hole formation channel between ∼12 and ∼15M ⊙discovered previously and implies that the black hole/neutron star birth ratio for solar-metallicity stars could be ∼20%. However, one channel leaves black holes in perhaps the ∼5–15M ⊙range with low kick speeds, while the other leaves black holes in perhaps the ∼2.5–3.0M ⊙mass range with high kick speeds. However, even ∼8.8 s after core bounce the newly formed black hole is still accreting at a rate of ∼2 × 10−2M ⊙s−1, and whether the black hole eventually achieves a significantly larger mass over time is yet to be determined. -
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