Neutron capture processes of heavy element synthesis

Details Neutron capture processes of heavy element synthesis Neutron capture processes of heavy element synthesis

Jan 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985aipc..124..504t&link_type=abstract

AIP Conference Proceedings, Volume 124, pp. 504-510 (1985).

Physics

Elementary Particle Processes, Stellar Structure, Interiors, Evolution, Nucleosynthesis, Ages

Scientific paper

The elements in nature which are heavier than iron are now understood to have been formed primarily by neutron-capture reaction mechanisms. Sequences of neutron captures, interspersed by beta decays, allow the buildup of progressively heavier nuclei. Solar system abundances reveal signatures of two such processes, distinguished by the conditions that the appropriate neutron capture timescales are greater than (s-process) or less than (r-process) the typical beta decay timescales in the vicinity of the valley of beta stability. The r-process flow paths can proceed into the neutron-rich regions far off the valley of beta stability, under some conditions even approaching the neutron-drip line, depending upon the prevailing neutron density and temperature. The s-process flow path is constrained rather to follow along the valley of beta stability. Observations and theory confirm the identification of the site of s-process synthesis with red giant stars. The site of r-process synthesis has not been unambiguously established. Recent studies of isotopic abundance anomalies in meteorites and of abundances in old and correspondingly metal deficient stars in our galaxy provide potentially important clues to the nature of the r-process site. Current theories of neutron capture synthesis will be reviewed.

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