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A Parametric Study of the Acoustic Mechanism for Core-collapse Supernovae

Harada, A. and Nagakura, H. and Iwakami, Wakana and Yamada, S. (2017) A Parametric Study of the Acoustic Mechanism for Core-collapse Supernovae. Astrophysical Journal, 839 (1). Art. No. 28. ISSN 1538-4357. doi:10.3847/1538-4357/aa6896.

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We investigate the criterion for the acoustic mechanism to work successfully in core-collapse supernovae. The acoustic mechanism is an alternative to the neutrino-heating mechanism. It was proposed by Burrows et al., who claimed that acoustic waves emitted by g-mode oscillations in proto-neutron stars (PNS) energize a stalled shock wave and eventually induce an explosion. Previous works mainly studied to which extent the g-modes are excited in the PNS. In this paper, on the other hand, we investigate how strong the acoustic wave needs to be if it were to revive a stalled shock wave. By adding the acoustic power as a new axis, we draw a critical surface, which is an extension of the critical curve commonly employed in the context of neutrino heating. We perform both 1D and 2D parametrized simulations, in which we inject acoustic waves from the inner boundary. In order to quantify the power of acoustic waves, we use the extended Myers theory to take neutrino reactions into proper account. We find for the 1D simulations that rather large acoustic powers are required to relaunch the shock wave, since the additional heating provided by the secondary shocks developed from acoustic waves is partially canceled by the neutrino cooling that is also enhanced. In 2D, the required acoustic powers are consistent with those of Burrows et al. Our results seem to imply, however, that it is the sum of neutrino heating and acoustic powers that matters for shock revival.

Item Type:Article
Related URLs:
URLURL TypeDescription
Nagakura, H.0000-0002-7205-6367
Iwakami, Wakana0000-0003-4959-069X
Yamada, S.0000-0002-2166-5605
Additional Information:© 2017 The American Astronomical Society. Received 2016 December 7; revised 2017 March 16; accepted 2017 March 20; published 2017 April 11. The authors thank Masataka Ogane for fruitful disucussion. A.H. also thanks Bernhard Müller for useful suggestion and discussion. Numerical computations were carried out on Cray XC30 at Center for Computational Astrophysics, National Astronomical Observatory of Japan, and the supercomputer system A at High Energy Accelerator Research Organization (KEK, support by the Large Scale Simulation Program No. 14/15-17 (FY2014-2015), No. 15/16-08 (FY2015-2016), and No. 16/17-11 (FY2016-2017)). A.H. is supported by Advanced Leading Graduate Course for Photon Science (ALPS) in the University of Tokyo. H.N. 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. This work was supported by the Grant-in-Aid for Scientific Research (B) (No. 16H03986) and Grant-in-Aid for Innovative Areas (No. 24103006) from the Ministry of Education, Culture, Sports, Science and Technology (MEXT), Japan.
Group:TAPIR, Walter Burke Institute for Theoretical Physics
Funding AgencyGrant Number
University of TokyoUNSPECIFIED
Japan Society for the Promotion of Science (JSPS)27-348
Ministry of Education, Culture, Sports, Science and Technology (MEXT)16H03986
Ministry of Education, Culture, Sports, Science and Technology (MEXT)24103006
Subject Keywords:methods: numerical – shock waves – supernovae: general
Issue or Number:1
Record Number:CaltechAUTHORS:20170411-092600583
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Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:76503
Deposited By: Tony Diaz
Deposited On:11 Apr 2017 16:49
Last Modified:15 Nov 2021 17:00

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