Fusion reactions of nuetron rich nuclei in dense matter

Details Fusion reactions of nuetron rich nuclei in dense matter Fusion reactions of nuetron rich nuclei in dense matter

Apr 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008aps..apr.d8001d&link_type=abstract

American Physical Society, 2008 APS April Meeting and HEDP/HEDLA Meeting, April 11-15, 2008, abstract #D8.001

Astronomy and Astrophysics

Astrophysics

Scientific paper

Fusion reactions play a key role in stellar evolution. The astrophysical S factor (or its associated fusion cross section) is important to know reaction rates, study chemical composition and temperature profiles of the star, as well as rate of production of heavy elements. There is not too much experimental information for the low energy fusion cross section of very neutron rich light nuclei. Using a simple barrier penetration model, we calculated the S factor for fusion reactions of neutron rich nuclei (^24O + ^24O, ^28Ne + ^28Ne and ^12C + a range of Oxygen isotopes up to ^24O). These results provide a lower limit for the fusion cross sections, since the dynamics of the neutron skin of neutron rich nuclei could enhance the penetration of the Coulomb barrier.

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