r-process nucleosynthesis in neutrino-driven winds from a typical neutron star with M = 1.4 M

M. Terasawa*, K. Sumiyoshi, S. Yamada, H. Suzuki, T. Kajino

*この研究の対応する著者

研究成果査読

38 被引用数 (Scopus)

抄録

We study the effects of the outer boundary conditions in neutrino-driven winds on r-process nucleosynthesis. We perform numerical simulations of hydrodynamics of neutrino-driven winds and nuclear reaction network calculations. As an outer boundary condition of hydrodynamic calculations, we set a pressure upon the outermost layer of the wind, which is approaching toward the shock wall. Varying the boundary pressure, we obtain various asymptotic thermal temperatures of expanding material in the neutrino-driven winds for resulting nucleosynthesis. We find that a slightly lower asymptotic temperature reduces the charged particle reaction rates and the resulting amount of seed elements and leads to a high neutron-to-seed ratio for a successful r-process abundance pattern, which is in reasonable agreement with the solar system r-process abundance pattern. As a result, the asymptotic temperature, slightly lower than those in previous studies of neutrino-driven winds, can lead to a successful r-process even for the typical proto-neutron star mass MNS ∼ 1.4 M. We also explore the relation between the boundary condition and the neutron star mass, which is related to the progenitor mass, for a successful r-process.

本文言語English
ページ(範囲)L137-L140
ジャーナルAstrophysical Journal
578
2 II
DOI
出版ステータスPublished - 2002 10 20
外部発表はい

ASJC Scopus subject areas

  • 天文学と天体物理学
  • 宇宙惑星科学

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