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On the importance of progenitor asymmetry to shock revival in core-collapse supernovae

Nagakura, Hiroki and Takahashi, Kazuya and Yamamoto, Yu (2019) On the importance of progenitor asymmetry to shock revival in core-collapse supernovae. Monthly Notices of the Royal Astronomical Society, 483 (1). pp. 208-222. ISSN 0035-8711. https://resolver.caltech.edu/CaltechAUTHORS:20190411-161323342

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Abstract

The progenitor stars of core-collapse supernovae (CCSNe) are asymmetrically fluctuating due to turbulent convections in the late stages of their lives. The progenitor asymmetry at the pre-supernova stage has recently caught the attention as a new ingredient to facilitate shock revival in the delayed neutrino-heating mechanism. In this paper, we investigate the importance of the progenitor asymmetries to shock revival with a semi-analytical approach. Free parameters were chosen such that the time evolution of shock radii and mass accretion rates are compatible with the results of detailed numerical simulations of CCSNe in spherical symmetry. We first estimate the amplitude of asymmetries required for the shock revival by the impulsive change of pre-shock flows in the context of neutrino-heating mechanism, and then convert the amplitude to the corresponding amplitude in the pre-supernova phase by taking into account the growth of asymmetries during infall. We apply our model to various types of progenitors and find that the requisite amplitude of pre-supernova asymmetry is roughly three times larger than the prediction by current stellar evolution models unless other additional physical ingredients such as multidimensional fluid instabilities and turbulent convections in post-shock flows aid shock revival. We thus conclude that progenitor asymmetries cannot trigger the shock revival by the impulsive way but rather play a supplementary role in reality.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1093/mnras/sty3114DOIArticle
ORCID:
AuthorORCID
Nagakura, Hiroki0000-0002-7205-6367
Additional Information:© 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model). Accepted 2018 November 12. Received 2018 November 12; in original form 2018 September 2. Published: 15 November 2018. We are grateful to Adam Burrows, Sherwood Richers, Jonathan Squire, and Wakana Iwakami for valuable comments on this paper. We also appreciate the anonymous referee for his/her comments, which crucially helped us to improve this paper. This work is partially supported by a Research Fellowship for Young Scientists from the Japan Society for the Promotion of Science (JSPS). HN was supported in part by JSPS Postdoctoral Fellowships for Research Abroad No. 27-348, and he was partially supported at Caltech through NSF award No. TCAN AST-1333520 and Princeton University through DOE SciDAC4 Grant DE-SC0018297 (subaward 00009650).
Group:TAPIR, Walter Burke Institute for Theoretical Physics
Funders:
Funding AgencyGrant Number
Japan Society for the Promotion of Science (JSPS)27-348
NSFAST-1333520
Department of Energy (DOE)DE-SC0018297
Department of Energy (DOE)00009650
Subject Keywords:turbulence – stars: evolution – supernovae: general
Issue or Number:1
Record Number:CaltechAUTHORS:20190411-161323342
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20190411-161323342
Official Citation:Hiroki Nagakura, Kazuya Takahashi, Yu Yamamoto, On the importance of progenitor asymmetry to shock revival in core-collapse supernovae, Monthly Notices of the Royal Astronomical Society, Volume 483, Issue 1, February 2019, Pages 208–222, https://doi.org/10.1093/mnras/sty3114
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:94676
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:12 Apr 2019 02:54
Last Modified:03 Oct 2019 21:06

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