Astronomy and Astrophysics – Astronomy
Scientific paper
May 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003sass...22...55m&link_type=abstract
The Society for Astronomical Sciences 22nd Annual Symposium on Telescope Science, held May 21-22, 2003. Published by Society for
Astronomy and Astrophysics
Astronomy
Scientific paper
Mira variable stars are a broad class of stars, which encompass spectroscopic classes of type M, S and C. These stars are closely related in terms of their long term variability, position on the Hertzsprung-Russell diagram their intermediate mass (from ~0.8 to ~8 solar mass) and the fact that class M evolves into the S and C type stars as certain stages of shell burning around the core proceeds. These shell burning episodes produce heavy elements beyond iron and also carbon which can appear at the surface of these stars during periods of convective instability resulting in greatly enhanced abundances of elements beyond the iron group and an increase in the carbon/oxygen ratio. In addition, it is suspected that these type stars, in particular, the M type Mira's can flare up over periods of hours to days by several tenths of a mag- nitude or more. The spectroscopic changes, which occur during these flare ep- isodes, ultimately driven by core burning evolution, remain relatively un- explored. This project was initiated in order to monitor a group of program stars of these classes in the V and R photometric bands in the hopes of "catching" some of these stars during one of these flare ups and thus to be able to conduct spectral analysis of the flare-ups in real time and compare these spectra to the non-flare spectra. This talk will describe the back- ground of these type stars, in particular, their evolutionary history and their spectroscopic differences. In addition, the strategies and initiation of this project will be described.
Mais Dale E.
Richards David
Stencel Robert E.
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