2021
DOI: 10.48550/arxiv.2112.09707
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Ninoy Rahman,
Hans-Thomas Janka,
Georg Stockinger
et al.

Abstract: We investigate the final collapse of rotating and non-rotating pulsational pair-instability supernova progenitors with zero-age-main-sequence masses of 60, 80, and 115 M and iron cores between 2.37 M and 2.72 M by 2D hydrodynamics simulations. Using the general relativistic NADA-FLD code with energy-dependent three-flavor neutrino transport by fluxlimited diffusion allows us to follow the evolution beyond the moment when the transiently forming neutron star (NS) collapses to a black hole (BH), which happens wi… Show more

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Cited by 2 publications
(2 citation statements)
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“…Furthermore, multiple PPI eruptions may be required to generate the large CSM mass covering radii ∼ 10 14 − 10 16 cm (potentially requiring a finetuned progenitor star mass), despite a broadly similar CSM density field now inferred to characterize multiple members of the LFBOT class (Ho et al 2019;Bright (Margutti et al 2019), is also in tension with the large ejecta masses predicted from the successful explosion of a ∼ 40M PPISN progenitor. The core collapse of stars which undergo PPI may not give rise to successful energetic SN explosions due to their massive Fe cores and the large gravitational binding energy of their envelopes (e.g., Powell et al 2021;Rahman et al 2021). An alternative, potentially more promising PPISN scenario for LFBOTs would therefore invoke an initially failed neutrino-driven explosion giving rise to prompt BH formation, followed by a delayed wind-driven explosion once the outer stellar layers form an accretion disk around the BH (similar to the scenario explored in Siegel et al 2021 in the context of even more massive stars above the pair-instability mass gap).…”
Section: Progenitor Modelsmentioning
confidence: 99%
“…It is assumed that less massive progenitors with zero-age main sequence (ZAMS) mass 20 M explode by the standard NDEmechanism (Nakamura et al 2015;Sukhbold et al 2016;Müller et al 2016;Burrows et al 2020), leaving behind NSs, while more massive stars usually collapse into BHs, even if shock revival may sometimes occur and be followed by a weak fallback explosion (e.g., Chan et al 2018Chan et al , 2020Ott et al 2018;Kuroda et al 2018;Powell et al 2021;Rahman et al 2021). So far, three-dimensional models of neutrino-driven explosions can only account for CCSNe of normal energies, not significantly exceeding 10 51 erg (Burrows et al 2020;Powell & Müller 2020;Bollig et al 2021).…”
Section: Introductionmentioning
confidence: 99%