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 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.
Stars:mass loss stars:AGB and post-AGB
Qian Wang Lee Anne Willson Steven Kawaler
Department of Physics and Astronomy,Iowa State University,Ames,IA 50010,USA
国际会议
The 252th Symposium of the International Astronomical Union(国际天文学联合会第252届研讨会)
海南三亚
英文
259-260
2008-04-06（万方平台首次上网日期，不代表论文的发表时间）