Final products of the rp-process on accreting neutron stars

Osamu Koike, Masa Aki Hashimoto, Reiko Kuromizu, Shin Ichirou Fujimoto

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37 Citations (Scopus)

Abstract

Using both shell-flash and realistic models on accreting neutron stars with the full nuclear reaction network up to Bi, we investigate the detailed relation between the final products of the rp-process and the ignition pressure. We find that nuclear fuels of H and 4He are almost burned out after the flash and that the mass number of synthesized nuclei reaches to ≃100 in the pressure range from 1023 to 1023.5 dyn cm -2 for a neutron star of 1.4 M and 10 km radius. Furthermore, p-nuclei up to 126Xe are found to be produced after the flash, thanks to our large network. The postprocess nucleosynthesis for accretion rates of 3 × 10-10, 3 × 10-9, and 10-8 M yr-1, which corresponds to an ignition pressure from 1022.7 to 1022.9 dyn cm -2, reveals that H is exhausted completely during the burst. This is because H decreases significantly as a result of the steady burning before the burst and convective mixing at the initial stage; we find that 64Zn is the most abundant element after the burst.

Original languageEnglish
Pages (from-to)242-251
Number of pages10
JournalAstrophysical Journal
Volume603
Issue number1 I
DOIs
Publication statusPublished - Mar 1 2004

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

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    Koike, O., Hashimoto, M. A., Kuromizu, R., & Fujimoto, S. I. (2004). Final products of the rp-process on accreting neutron stars. Astrophysical Journal, 603(1 I), 242-251. https://doi.org/10.1086/381354