TP-AGB evolution with overshoot for low-mass stars as a function of metallicity

F. Herwig1, T. Blöcker2, T. Driebe2

1Universität Potsdam, Institut für Physik, Astrophysik
2Max Planck Institut für Radioastronomie, Bonn

We give a brief review on the properties of asymptotic giant branch models with overshoot. Then we describe new model calculations with overshoot. Initial masses are ranging from 1 to 3 Msun and metallicities are Z=0.02, 0.01 and 0.001. Third dredge-up occurs efficiently for low masses and carbon stars are formed, with some at core masses as low as 0.58 Msun. After the thermal pulse at which stars become C-rich the luminosities are in the range of the observed C-star luminosity function during the whole interpulse phase and for all C-star models. The dredge-up evolution depends mainly on the core mass at the first thermal pulse and on the metallicity. The Z=0.001 models of the 2 and 3 Msun sequence become C-rich almost instantaneously after the onset of the first thermal pulses. For the 2 Msun case the C/O ratio initially exceeds 4. During following dredge-up episodes the C/O ratio decreases

The full article is available as PostScript file via anonymous ftp.
user: anonymous or ftp; Password: your e-mail address;
file: pub/herwig/PUBLIKATIONEN/ (324kB uncompressed or (53kB compressed).

Display full article with ghostview (local users only!)

Fetch PostScript-File (, 324kB, uncompressed)

Fetch PostScript-File (, 53kB, compressed)

Zurück zur Übersicht