Synoptic APT Photometry of the RS CVn Binary HD 28591

Details Synoptic APT Photometry of the RS CVn Binary HD 28591 Synoptic APT Photometry of the RS CVn Binary HD 28591

Dec 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...181.6608s&link_type=abstract

American Astronomical Society, 181st AAS Meeting, #66.08; Bulletin of the American Astronomical Society, Vol. 24, p.1225

Astronomy and Astrophysics

Astronomy

Scientific paper

HD 28591 is a single-lined, non-eclipsing RS CVn binary which exhibits photometric variations indicative of starspot activity. We report on B and V observations obtained over the period 1988-1992 with the Phoenix-10 Automatic Photoelectric Telescope sited on Mt. Hopkins, AZ. The system exhibits a variable distortion wave with amplitudes ranging from 0.04 to 0.07 magnitudes in V as well as a variable mean light level. A Scargle periodogram analysis of the entire dataset shows a highly significant peak at a period of 10.650 days. As this is exactly half the reported orbital period of 21.3 days, this casts doubt on its validity as the rotational period of the primary. Inspection of the differential magnitudes plotted against J. D. as well as light curves phased with both periods leaves little doubt that the star is synchronously rotating but with a light curve that shows two, often unequal, maxima per orbit. We have modelled the B and V data simultaneously using the formalism of Budding (1977). This analysis indicates that two distinct spot groups, widely separated in longitude, are needed during all seasons to accurately model the light curves. The results for the individual years show evolution over time of both the spot sizes and longitudes. The measurement of the total spotted areas in these seasons ranges from approximately 0.017 to 0.034 of the total surface area and shows some preliminary indications of a starspot cycle in HD 28591.

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