The reaction rate for the destruction of fluorine in AGB stars

Details The reaction rate for the destruction of fluorine in AGB stars The reaction rate for the destruction of fluorine in AGB stars

Jul 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005nupha.758..577u&link_type=abstract

Nuclear Physics A, Volume 758, p. 577-580.

Physics

Nuclear Physics

1

Scientific paper

The 19F(α, p)22Ne reaction is considered to be the main source of fluorine depletion during the Asymptotic Giant Branch phase in stars. The reaction rate still retains large uncertainties due to the lack of experimental studies available. The yields for both the ground p0 and first excited state p1 exit channels of 22Ne have been measured with the University of Notre Dame KN van de Graaff accelerator. Ten resonances were found in the energy range E=990 1570 keV and their strengths have been determined. A comparison between the rate calculated from the experimental data and other standard rates is provided.

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