Mass loss from pulsating cool stars

It has long been clear that most, if not all, of the mass loss experienced by stars from 0.8 to 8 solar masses occurs near the tip of the AGB and/or the RGB. Evolutionary studies have incorporated empirical mass loss laws but theoretical models suggest quite different dependence of mass loss rate on...

Full description

Saved in:
Bibliographic Details
Published in:Proceedings of the International Astronomical Union 2008-04, Vol.4 (S252), p.259-260
Main Authors: Wang, Qian, Willson, Lee Anne, Kawaler, Steven
Format: Article
Language:English
Subjects:
Astronomical models
Astronomy
Astrophysics
Contributed Papers
Cool stars
Metallicity
Stars & galaxies
Stellar evolution
Citations: Items that this one cites
Online Access:Get full text
Tags: Add Tag
No Tags, Be the first to tag this record!
Description
Summary:It has long been clear that most, if not all, of the mass loss experienced by stars from 0.8 to 8 solar masses occurs near the tip of the AGB and/or the RGB. Evolutionary studies have incorporated empirical mass loss laws but theoretical models suggest quite different dependence of mass loss rate on stellar parameters. We are combining evolutionary model calculations with ISUEVO with mass loss modeling using the Bowen code in a systematic study of final stages of stellar evolution. We mapped the RGB (without steady mass loss) to the “Death Zone” as a function of mixing length, mass, and metallicity. We compared these results with observation data from Origlia. We are investigating a possible mass loss mechanism through companions as a complement to mass loss through pulsation. By the end of the project we expect to provide a reliable prescription for AGB mass loss.
ISSN:1743-9213
1743-9221
DOI:10.1017/S1743921308022953