Effective resonant formation of 20Ne in stars

✍ Scribed by A. E. Md. Khairozzaman

• Publisher: John Wiley and Sons
• Year: 1986
• Tongue: English
• Weight: 218 KB
• Volume: 307
• Category: Article
• ISSN: 0004-6337
• DOI: 10.1002/asna.2113070404

✦ Synopsis

l h c resonant reaction rates of I60(a, y)"Ne have been determined for tlic 5.64(3-) b1cV and 5.8(1-) MeV excited stales of "lie uritlcr strong screening conditions utilizing the teniperature-density plots of the helium plasma after ITOH ct al. (1977). 'The screened reaction rates wcre found to be ixany times groater than the unscreened ones. It has been iound that the most effective resonant formation of 2 0 N ~ takes place a t density I O ~ g ~r n -~.

As the density increases beyond 1oE g c ~n -~ with corresponding rise of temperature thc screened reaction rates (i. e. effective reaction rates) decrease. Such a decrease affects the presupernova yields from massive stars drastically The giant and dwarf stage of stellar evolution under pycnonnclcar density conditioiis ( 1 0 ~-109 g ~m -~) will be retarded beyond the density of 108 g cm-3 in stellar interiors.