Nucleosynthesis in neutrino-driven winds: II. Implications for heavy element synthesis

Details Nucleosynthesis in neutrino-driven winds: II. Implications for heavy element synthesis Nucleosynthesis in neutrino-driven winds: II. Implications for heavy element synthesis

1996-11-13

arxiv.org/abs/astro-ph/9611097v1

Astrophys.J.482:951,1997

Astronomy and Astrophysics

Astrophysics

36 pages, 11 Postscript figures, AASTex

Scientific paper

10.1086/304181

During the first 20 seconds of its life, the enormous neutrino luminosity of a neutron star drives appreciable mass loss from its surface. This neutrino-driven wind has been previously identified as a likely site for the r-process. Qian & Woosley (1996) have derived, both analytically and numerically, the physical conditions relevant for heavy element synthesis in the wind. These conditions include the entropy (S), the electron fraction (Ye), the dynamic time scale, and the mass loss rate. Here we explore the implications of these conditions for nucleosynthesis. We find that the standard wind models derived in that paper are inadequate to make the r-process, though they do produce some rare species above the iron group. We further determine the general restrictions on the entropy, the electron fraction, and the dynamic time scale that are required to make the r-process. In particular, we derive from nuclear reaction network calculations the conditions required to give a sufficient neutron-to-seed ratio for production of the platinum peak. These conditions range from Ye = 0.2 and S < 100 per baryon for reasonable dynamic time scales of 0.001-0.1 s, to Ye = 0.4-0.495 and S > 400 per baryon for a dynamic time scale of 0.1 s. These conditions are also derived analytically to illustrate the physics determining the neutron-to-seed ratio.

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