A Possible Criterion for Envelope Ejection in Asymptotic Giant Branch or First Giant Branch Stars

Details A Possible Criterion for Envelope Ejection in Asymptotic Giant Branch or First Giant Branch Stars A Possible Criterion for Envelope Ejection in Asymptotic Giant Branch or First Giant Branch Stars

Sep 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994mnras.270..121h&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Vol. 270, NO. 1/SEP1, P. 121, 1994

Astronomy and Astrophysics

Astronomy

166

Scientific paper

Following Paczyriski & Zi6ikowski, we investigate the relationship between the zero- age mass of a star and the mass of its degenerate core at that point in the star's evolution when the binding energy of its envelope changes from negative to positive. This relationship is fairly consistent, to within observational error, with the relationship by Weidemann & Koester between the initial mass and the mass of the white dwarf (WD) remnant, and with the observed distribution of masses of planetary nebula nuclei. We derive the equivalent relation for Population II (Pop II) stars (Z = 0.001), finding white dwarf masses 10-20 per cent greater for the same initial masses. For both Population I (Pop I) and Pop II, however, we do not obtain CIG WD masses above 1.1 M0 - the putative massive progenitors (> 8 and 6 M0 respectively) have negative envelope binding energies even at fairly extreme red supergiant radii. For low-mass Pop I stars (< 1 M0), we obtain He WD remnants by the same process on the first giant branch. We discuss the implications of our calculations for C/O WD masses, thermonuclear Type II supernovae, and the use of planetary nebulae as distance candles. Key words: stars: AGB and post-AGB - stars: evolution - stars: mass-loss - white dwarfs - planetary nebulae: general.

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