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Light elements synthesized in the He-layer and the H-rich envelope of a type II supernova, II, —Influence of initial chemical compositions—

Earth, Planets and Space volume 52, pages 361–376 (2000)Cite this article

Abstract

This is the second paper of a series of our studies, in which we have investigated the light element synthesis (Li, Be, B, and the CNO-elements) in the He-layer and the H-rich envelope of supernovae and the aim of this paper is to see the sensitivity of the element synthesis to the chemical compositions in the presupernova stage. First, we deduced the probable range of the chemical composition in the presupernova stage on the basis of the previous studies of stellar evolution as well as the observational studies of stellar chemical compositions. Secondly, we pursued the explosive nucleosynthesis by using artificially modeled chemical compositions composed of only four elements (1H, 4He, 12C, and 16O). Combining these results, we constructed five kinds of diagrams between two isotopic/elemental ratios which are useful for distinguishing presolar grains of supernova origin: 6Li/16O and 9Be/16O to 7Li/16O, and 11B/7Li, 14N/15N, and 16O/17O to 12C/(13C. In conclusion, the uncertainties in the chemical compositions in the presupernova stage brought smaller varieties in the isotopic/elemental ratios of the light elements compared with the varieties investigated in our first paper about the neutrino emission models.

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Author notes

  1. Takashi Yoshida

    Present address: Department of Physics, Kyushu University, Chuo-ku, Fukuoka, 810-8560, Japan

Authors and Affiliations

  1. Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Meguro-ku, Tokyo, 152-8551, Japan

    Takashi Yoshida, Kiyoshi Nakazawa & Hiroyuki Emori

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  1. Takashi Yoshida
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  2. Kiyoshi Nakazawa
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  3. Hiroyuki Emori
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Correspondence to Takashi Yoshida.

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Yoshida, T., Nakazawa, K. & Emori, H. Light elements synthesized in the He-layer and the H-rich envelope of a type II supernova, II, —Influence of initial chemical compositions—. Earth Planet Sp 52, 361–376 (2000). https://doi.org/10.1186/BF03351648

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