News from r-Process Nucleosynthesis: Consequences from the ESS to Early Stars

Details News from r-Process Nucleosynthesis: Consequences from the ESS to Early Stars News from r-Process Nucleosynthesis: Consequences from the ESS to Early Stars

Apr 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008aipc.1001..245f&link_type=abstract

IXTH TORINO WORKSHOP ON EVOLUTION AND NUCLEOSYNTHESIS IN AGB STARS AND THE IIND PERUGIA WORKSHOP ON NUCLEAR ASTROPHYSICS. AIP C

Astronomy and Astrophysics

Astrophysics

4

Stellar Structure, Interiors, Evolution, Nucleosynthesis, Ages, Supernovae, Abundances, Chemical Composition

Scientific paper

The exact conditions for the supemova high-entropy wind (HEW) as one of the favored sites for the rapid neutron-capture (r-) process still cannot be reproduced self-consistently in present hydrodynamic astrophysical models. Therefore, we have performed large-scale dynamical network calculations within a parameterized HEW model to constrain the necessary conditions for a full r-process and to compare our results with recent observations. A model-inherently weighted superposition of entropy trajectories results in an excellent reproduction of the overall Solar-System isotopic abundances (Nr,solar) of the ``main'' r-process elements beyond Sn. For the lighter r-elements in the range 26<=Z<=42, our HEW model supports earlier qualitative ideas about a multiplicity of nucleosynthetic processes leading to the total Nr,solar distribution. In the HEW scenario, these suggestions are quantified, and the origin of the missing primary process is confirmed to be a rapid charged-particle process, thus excluding a ``weak'' neutron-capture component. This explains the recent halo-star observations of a Z-dependent non-correlation, respectively partial correlation of the lighter r-elements with metallicity and/or enrichment of ``main'' r-process elements.

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