Supernovae versus Neutron Star Mergers as the Major r-Process Sources

Details Supernovae versus Neutron Star Mergers as the Major r-Process Sources Supernovae versus Neutron Star Mergers as the Major r-Process Sources

2000-03-16

arxiv.org/abs/astro-ph/0003242v1

Astrophys.J. 534 (2000) L67-L70

Astronomy and Astrophysics

Astrophysics

5 pages, to appear in ApJL

Scientific paper

10.1086/312659

I show that recent observations of r-process abundances in metal-poor stars are difficult to explain if neutron star mergers (NSMs) are the major r-process sources. In contrast, such observations and meteoritic data on Hf182 and I129 in the early solar system support a self-consistent picture of r-process enrichment by supernovae (SNe). While further theoretical studies of r-process production and enrichment are needed for both SNe and NSMs, I emphasize two possible direct observational tests of the SN r-process model: gamma rays from decay of r-process nuclei in SN remnants and surface contamination of the companion by SN r-process ejecta in binaries.

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