On the importance of progenitor asymmetry to shock revival in core-collapse supernovae
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.
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).Attached Files
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Additional details
- Eprint ID
- 94676
- Resolver ID
- CaltechAUTHORS:20190411-161323342
- 27-348
- Japan Society for the Promotion of Science (JSPS)
- AST-1333520
- NSF
- DE-SC0018297
- Department of Energy (DOE)
- 00009650
- Department of Energy (DOE)
- Created
-
2019-04-12Created from EPrint's datestamp field
- Updated
-
2021-11-16Created from EPrint's last_modified field
- Caltech groups
- TAPIR, Walter Burke Institute for Theoretical Physics