The Chemical Evolution in the Solar Vicinity and the Nucleosynthesis of Neutron Capture Elements

Details The Chemical Evolution in the Solar Vicinity and the Nucleosynthesis of Neutron Capture Elements The Chemical Evolution in the Solar Vicinity and the Nucleosynthesis of Neutron Capture Elements

Apr 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008aipc.1001...63c&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

Galactic Halo, Abundances, Chemical Composition, Stellar Structure, Interiors, Evolution, Nucleosynthesis, Ages

Scientific paper

We propose an explanation for the considerable scatter of the abundances of neutron capture elements observed in low metallicity stars in the solar vicinity, compared to the small star to star scatter observed for the α-elements. We have developed a stochastic chemical evolution model, in which the main assumption is a random formation of new stars, subject to the condition that the cumulative mass distribution follows a given initial mass function. With our model we are able to reproduce the different spreads of neutron capture elements and α-elements in low metallicity stars. The reason for different observed spread in neutron capture elements and α-elements resides in the random birth of stars coupled with different stellar mass ranges from which α-elements and neutron capture elements originate. In particular, the site of production of α-elements is the whole range of the massive stars, from 10 to 8OMsolar whereas the mass range of production for neutron capture elements lies between 12 and 30Msolar.

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