2021
DOI: 10.1093/mnras/stab614 View full text |Buy / Rent full text
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Abstract: We present 3D core-collapse supernova simulations of massive Pop-III progenitor stars at the transition to the pulsational pair instability regime. We simulate two progenitor models with initial masses of 85 M⊙ and 100 M⊙ with the LS220, SFHo, and SFHx equations of state. The 85 M⊙ progenitor experiences a pair instability pulse coincident with core collapse, whereas the 100 M⊙ progenitor has already gone through a sequence of four pulses 1,500 years before collapse in which it ejected its H and He envelope. T… Show more

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“…Interestingly, Powell et al (2021) witnessed shock revival by neutrino heating prior to BH formation in their models, in line with results of various other studies of the collapse of massive stars with 𝑀 ZAMS ≥ 40 M to BHs (e.g., Kuroda et al 2018;Summa et al 2018;Ott et al 2018;Pan et al 2018Pan et al , 2021Burrows et al 2020;Chan et al 2018. The neutrino energy transfer increases for more compact NSs and with longer time span between shock revival and the collapse of the transiently stable NS to a BH.…”
Section: Introductionsupporting
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“…Interestingly, Powell et al (2021) witnessed shock revival by neutrino heating prior to BH formation in their models, in line with results of various other studies of the collapse of massive stars with 𝑀 ZAMS ≥ 40 M to BHs (e.g., Kuroda et al 2018;Summa et al 2018;Ott et al 2018;Pan et al 2018Pan et al , 2021Burrows et al 2020;Chan et al 2018. The neutrino energy transfer increases for more compact NSs and with longer time span between shock revival and the collapse of the transiently stable NS to a BH.…”
Section: Introductionsupporting
“…Chan et al (2018) studied the core collapse of a metal-free progenitor with a ZAMS mass of 40 M from Heger & Woosley (2010). Kuroda et al (2018) 2018), however employing different nuclear EOSs, namely LS220 (the same EOS as used by Chan et al 2018;Powell et al 2021 andKuroda et al 2018), SFHo (this EOS is used in our study as well as by Powell et al 2021), DD2 (Fischer et al 2014), and BHBΛ𝜙 (Banik et al 2014). Chan et al (2018) fostered shock revival in their 40 M simulation by artificially increasing the strangeness contribution to the axial-vector coupling for neutral-current neutrino-nucleon scattering, using a coupling constant of 𝑔 A,s = −0.2, which is on the extreme side compared to experimental and theoretical constraints (see Hobbs et al 2016).…”
Section: Comparison With Previous Workmentioning
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“…Hence, adopting the PPISN interpretation likely requires that the ejecta be highly aspherical (e.g., a bipolar jet-driven outflow) or that nearly all of the star collapses into a black hole and only a small fraction is ejected (see, e.g., Wongwathanarat et al 2013 for aspherical mass ejection in the neutron star case.) Powell et al (2021) examines core collapse and the (partial) explosion of PPISN models. For their low-mass PPISN model, a successful explosion of ∼3 × 10 51 erg is observed but the high binding energy of the remnant implies black hole formation with partial mass ejection.…”
Section: Asphericity and Jet-like Explosionmentioning