Spectroscopic Monitoring of Mira-type and Semi-regular Variable Stars

Details Spectroscopic Monitoring of Mira-type and Semi-regular Variable Stars Spectroscopic Monitoring of Mira-type and Semi-regular Variable Stars

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...211.6018v&link_type=abstract

American Astronomical Society, AAS Meeting #211, #60.18; Bulletin of the American Astronomical Society, Vol. 39, p.846

Astronomy and Astrophysics

Astronomy

Scientific paper

With the rise in availability of spectroscopic equipment for smaller telescopes, comprehensive phase-dependent spectroscopic monitoring of variable stars has become a reality. Pulsating variable stars on the asymptotic giant branch (AGB), including both long period Mira-type variables and smaller amplitude semi-regular variables, are known to have complex atmospheric structures that contain heavier elements and molecules characteristic of cooler, late-life stars. Spectroscopic measurements taken at regular intervals over their pulsation cycle reveal changes in spectral features over time, such as changes in molecular band strengths and transitions from absorption to emission in the Hydrogen Balmer series. We have begun a program of spectroscopic monitoring of AGB variables at both 4-Angstrom and 1-Angstrom resolution in order to catalog and quantify changes in their spectra as a function of phase. Spectra taken at approximately 10-day intervals for the Mira-type variables RT Cygni and X Ophiuchi, and for the semi-regular variables RZ Arietis and AV Arietis along with a preliminary analysis will be presented.
This research was supported by the National Science Foundation under Grant No. 0431664 and by the American Astronomical Society Small Research Grant program.

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