Helium in Planetary Nebulae and Asymptotic Giant Branch Models

Details Helium in Planetary Nebulae and Asymptotic Giant Branch Models Helium in Planetary Nebulae and Asymptotic Giant Branch Models

Dec 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994aas...185.4714b&link_type=abstract

American Astronomical Society, 185th AAS Meeting, #47.14; Bulletin of the American Astronomical Society, Vol. 26, p.1386

Astronomy and Astrophysics

Astronomy

Scientific paper

New grids of models of thermally pulsing asymptotic giant branch (AGB) stars are calculated using the method of Renzini and Voli (1981) to follow the surface abundances of (1) H, (4) He, (12) C, (13) C, (14) N, and (16) O over time. We use a new relation for the luminosity, based on the recent AGB models (Blocker and Schonberner (1991); Boothroyd and Sackmann (1988, 1992); Boothroyd, Sackmann and Ahern (1993); Lattanzio (1992); and Vassilidias and Wood (1993)). The mass loss from the AGB is parameterized using the relations given by Vassiliadis and Wood (1993). The predicted abundance ratios of He/H are compared to those observed in planetary nebulae. The yield of (4) He from 1-8Msun stars is discussed.

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