Surface Activity Analysis of the Eclipsing Binary UV Leonis Based On New Spectrophotometric Data

Details Surface Activity Analysis of the Eclipsing Binary UV Leonis Based On New Spectrophotometric Data Surface Activity Analysis of the Eclipsing Binary UV Leonis Based On New Spectrophotometric Data

Jan 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21541936c&link_type=abstract

American Astronomical Society, AAS Meeting #215, #419.36; Bulletin of the American Astronomical Society, Vol. 42, p.282

Astronomy and Astrophysics

Astronomy

Scientific paper

UV Leonis is an eclipsing binary system consisting of two type G stars with a period of 0.6 days. Evidence has been found of a period change in 1980, as previously reported by Wunder (1995) and Snyder (1998), but the exact nature and cause is still debatable. Stellar activity models have been explored by Frederik and Etzel (1996) but should be reexamined in light of more recent observations. Additional spectroscopic and photometric data were acquired by Kjurkchieva and Marchev (2007) but stellar activity was not analyzed. In an attempt to gain better insight into the period change and stellar activity, we have obtained forty nights of photometric data from the 30” Automated Photoelectric Telescope in Patagonia, Arizona and have used echelle spectra from the 1.8m Mt. Ekar telescope in Asiago, Italy. We propose a stellar activity model with two spots about the same size as in the previous model, but with spot-to-photosphere temperature ratios of about 0.95 instead of 0.8. As opposed to two polar spots, our model consists of two migrating equatorial spots on the primary star.

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