Pair-instability Supernova Simulations: Progenitor Evolution, Explosion, and Light Curves

Gilmer, Matthew S.; Kozyreva, Alexandra; Hirschi, Raphael; Fröhlich, Carla; Yusof, Norhasliza

doi:10.3847/1538-4357/aa8461

Title: Pair-instability Supernova Simulations: Progenitor Evolution, Explosion, and Light Curves

Journal Article · Wed Sep 06 00:00:00 EDT 2017 · The Astrophysical Journal (Online)

DOI:https://doi.org/10.3847/1538-4357/aa8461· OSTI ID:1537193

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^[2]; Hirschi, Raphael ^[3];

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North Carolina State Univ., Raleigh, NC (United States). Dept. of Physics
Tel Aviv Univ., Tel Aviv (Israel). The Raymond and Beverly Slacker School of Physics and Astronomy
Keele Univ., Keele, Staffordshire (United Kingdom). School of Chemical and Physical Sciences, Astrophysics group; Univ. of Tokyo, Kashiwa, Chiba (Japan). Univ. of Tokyo Inst. for Advanced Study, Kavli Inst. for the Physics and Mathematics of the Universe (WPI)
Univ. of Malaya, Kuala Lumpur (Malaysia). Dept. of Physics, Faculty of Science

Recently, the viability of the pair-instability supernova (PISN) scenario for explaining superluminous supernovae has all but disappeared except for a few slowly-evolving examples. However, PISNe are not predicted to be superluminous throughout the bulk of their mass range. In fact, it is more likely that the first PISN we see (if we have not seen one already) will not be superluminous. Here, we present hydrodynamic simulations of PISNe for four stellar models with unique envelope properties spanning the PISN mass range. In addition, we compute synthetic light curves (LCs) for comparison with current and future observations. We also investigate, in the context of our most massive model, the prospect of mixing in the supernova ejecta, alleviating discrepancies between current PISN models and the remaining superluminous candidate events. To this end, we present the first published 3D hydrodynamic simulations of PISNe. After achieving convergence between 1D, 2D, and 3D simulations, we examine mixing in the supernova ejecta and its affect on the bolometric LC. We observe slight deviations from spherical symmetry, which increase with the number of dimensions. We find no significant effects on the bolometric LC; however, we conclude that mixing between the silicon and oxygen rich layers caused by the Rayleigh–Taylor instability may affect spectra.

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Research Organization:: North Carolina State University, Raleigh, NC (United States)

Sponsoring Organization:: USDOE Office of Science (SC)

Grant/Contract Number:: SC0010263

OSTI ID:: 1537193

Journal Information:: The Astrophysical Journal (Online), Vol. 846, Issue 2; ISSN 1538-4357

Publisher:: Institute of Physics (IOP)Copyright Statement

Country of Publication:: United States

Language:: English

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Cited by: 25 works

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