Simultaneous Hα spectroscopy and CCD photometry in BVRI are used to model variable line emission in the eclipsing binary FF Aqr, which consists of a G subgiant and a hot subdwarf in a 9.2 day orbit. We modeled the phase dependent Hα emission as chromospheric fluorescence on the red star. The photometry is used to identify any other effects caused by the intrinsic activity of the cool star. The observations were part of a 12 night campaign on several chromospherically active binaries with the SARA 0.9m and Coude Feed telescopes at Kitt Peak National Observatory. We would like to thank the Southeastern Association for Research in Astronomy for their support and use of the SARA telescope and KPNO for funding the observer at the Coude Feed.
American Astronomical Society Meeting Abstracts #194
- Pub Date:
- May 1999