Starspot photometry with robotic telescopes^*

Continuous UBV and photometry of 23 stars in 1991–1996

¹ Institut für Astronomie, Universität Wien, Türkenschanzstraße 17, A-1180 Wien, Austria strassmeier@astro.ast.univie.ac.at
² Konkoly Observatory, Hungarian Academy of Sciences, H-1525 Budapest, Hungary bartus@buda.konkoly.hu
³ Catania Astrophysical Observatory, V.le A. Doria 6, I-95125 Catania, Italy

Received: 23 September 1996
Accepted: 16 December 1996

Abstract

We report on the progress of our ongoing photometric monitoring program of spotted late-type stars with automatic photoelectric telescopes (APTs) on Mt. Hopkins in Arizona and on Mt. Etna in Sicily. We present 9 250 differential UBV and/or observations for altogether 23 chromospherically active stars, singles and binaries, pre main sequence and post main sequence, taken between 1991 and 1996. The variability mechanism of our target stars is mostly rotational modulation by an asymmetrically spotted stellar surface. Therefore, precise rotational periods and their seasonal variations are determined using baselines between 3 years for HD 129333 to 34 years for V410 Tauri. We report the largest V light-curve amplitude of any spotted star observed to date: for V410 Tau in 1994–95. Long-term variations of the overall light levels of our target stars are sometimes of similar amplitude as the rotational modulation itself and are most likely caused by an analog of the solar 11-year spot cycle but mostly without a well-defined periodicity. For some of our target stars (HD 12545, HD 17433, EI Eri, V410 Tau, LQ Hya, and HD 106225) we estimate a probable cycle period. A complete light curve of the semi-regular S-type giant HR Pegasii is presented. All data are available via the WorldWideWeb.