Bulletin of the American Physical Society
6th Joint Meeting of the APS Division of Nuclear Physics and the Physical Society of Japan
Sunday–Friday, November 26–December 1 2023; Hawaii, the Big Island
Session E09: Nuclear Astrophysics III
7:00 PM–9:15 PM,
Wednesday, November 29, 2023
Hilton Waikoloa Village
Room: Kohala 2
Chair: Andrew Ratkiewicz, Lawrence Livermore National Laboratory
Abstract: E09.00003 : 56Ni Problem in Core-collapse Supernova Explosion*
7:30 PM–7:45 PM
Presenter:
RYO SAWADA
(The University of Tokyo)
Authors:
RYO SAWADA
(The University of Tokyo)
Yudai Suwa
(The University of Tokyo)
Recently, however, some studies have suggested that this 56Ni problem is derived from the simplicity of the explosion model [3]. In response, we investigate the effect of the explosion energy growth rate on the behavior of nucleosynthesis in CCSNe in a more realistic model [4]. We employ the 1D Lagrangian hydrodynamic code, in which we take neutrino heating and cooling terms into account with the light-bulb approximation. We reiterate that, consistent with previous rebuttal studies, there is the 56Ni problem: Although 56Ni is synthesized to almost the same mass coordinate independent of the energy growth rates, some of the innermost material in the low rate model failed to escape, leading to a shift in the innermost mass coordinate of the ejecta to the outer positions.
Comparing our results with observations, we find that while modern slow explosions can, in principle, reproduce observations of standard Type II SNe, this is not possible with stripped-envelope SNe. Our finding places a strong constraint on the explosion mechanism and suggests new directions for unraveling astrophysics from a nuclear physics perspective.
[1] R. Bollig et al., The Astrophysical Journal 915, 28 (2021).
[2] R. Sawada and K. Maeda, The Astrophysical Journal 886, 47 (2019).
[3] L. Imasheva, H.-T. Janka, and A. Weiss, Monthly Notices of the Royal Astronomical Society 518, 1818 (2022).
[4] R. Sawada and Y. Suwa, eprint arXiv:2301.03610 (2023).
*The work has been supported by Japan Society for the Promotion of Science (JSPS) KAKENHI grants 21J00825, 21K13964 (RS), 18H05437, 20H00174, 20H01904, and 22H04571 (YS).
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