Other
Scientific paper
Sep 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aspc..412..137w&link_type=abstract
The Biggest, Baddest, Coolest Stars ASP Conference Series, Vol. 412, proceedings of the workshop held 16-18 July 2007, at the Mi
Other
3
Scientific paper
We look to observations to tell us the dependence of mass loss rates on stellar parameters - L, R, M, T_{eff}, and Z - but what observations of mass loss rates tell us instead is the parameters of stars that have reached an interesting rate of mass loss. In order to find the dependence of the mass loss rates on stellar parameters - the slopes d log dot M/d log L along an evolutionary track, d log dot M/d log M, and for some situations also d log dot M/d log R or d log dot M/d log T_{eff} - we need to look to other kinds of data, such as the distribution of stars vs. luminosity or mass loss rate or radius or pulsation period, or the duration of the mass loss process. Mass loss from the biggest, coolest stars is highly sensitive to the stellar parameters, and this results in a narrow ``death zone" of mass loss rates sufficient to strip the star of its envelope. Recognizing this pattern, we can draw some strong conclusions about mass loss on the AGB, and also on the RGB, for various populations.
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