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Non-exploding and exploding core-collapse supernova models and the multimessenger predictions

Published online by Cambridge University Press:  12 October 2020

Kei Kotake Open the ORCID record for Kei Kotake [Opens in a new window] ,
Takami Kuroda  and
Tomoya Takiwaki
Kei Kotake
Affiliation:
Department of Applied Physics & Research Institute of Stellar Explosive Phenomena, Fukuoka University, Jonan, Nanakuma, Fukuoka814-0180, Japan
Takami Kuroda
Affiliation:
Institute für Kernphysik, Technische Universität Darmstadt, D-64289 Darmstadt, Germany
Tomoya Takiwaki
Affiliation:
Division of Theoretical Astronomy, National Astronomical Observatory of Japan, 2-21-1, Osawa, Mitaka, Tokyo, 181-8588, Japan
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Abstract

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We present results of full general relativistic (GR), three-dimensional (3D) core-collapse simulation of a massive star with multi-energy neutrino transport. Using a 70Mȯ zero-metallicity star, we show that the black-hole (BH) formation occurs at ∼ 300 ms after bounce. At a few ∼ 10 ms before the BH formation, we find that the stalled bounce shock is revived by neutrino heating from the forming hot proto-neutron star (PNS), which is aided by vigorous convection behind the shock. Our numerical results present the first evidence to validate the BH formation by the so-called fallback scenario. Furthermore we present results from a rapidly rotating core-collapse model of a 27Mȯ star that is trending towards an explosion. We point out that the correlated neutrino and gravitational-wave signatures, if detected, could provide a smoking-gun evidence of rapid rotation of the newly-born PNS.

Keywords

supernovae:generalhydrodynamicsintabilitiesneutrinosgravitational waves
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 15 , Symposium S350: Laboratory Astrophysics: From Observations to Interpretation , April 2019 , pp. 267 - 273
Copyright
© International Astronomical Union 2020

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