Astron. Astrophys. 347, 572-582 (1999)

Footnotes

1. This electronic address also provides many other nuclear data of nuclear astrophysics interest

2. Arnould et al. (1995) have reached a different conclusion due to a trivial mistake in the rate used in their calculations

3. In detailed stellar models, the temperature increases to values in excess of towards the end of core (or shell) He-burning. This may lead to the destruction of by (with a concomitant production of neutrons) or reactions, as illustrated on Fig. 11b

© European Southern Observatory (ESO) 1999

Online publication: June 30, 1999
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