The long-period RS CVn binary IM Pegasi --- II. First surface images

Details The long-period RS CVn binary IM Pegasi --- II. First surface images The long-period RS CVn binary IM Pegasi --- II. First surface images

Aug 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000a%26a...360..272b&link_type=abstract

Astronomy and Astrophysics, Vol. 360, p.272-280

Astronomy and Astrophysics

Astrophysics

22

Stars: Imaging, Stars: Starspots, Stars: Activity, Stars: Late-Type, Stars: Individual: Im Peg

Scientific paper

New high-resolution, high signal-to-noise ratio spectroscopic observations and UBV photometry carried out in 1996-1999 were analysed with the surface imaging technique. A total of 8 images of IM Peg was obtained for the first time. A huge high-latitude active region was found to dominate the stellar surface and decreased in area during the period of the observations. At the same time, on the opposite hemisphere (in longitudes), smaller spots were developing. The spots were migrating in the orbital reference frame, the period of spot rotation being of 24.d73∓0.d02. The spots constitute two active longitudes on opposite stellar hemispheres, similar to other RS CVn stars. The evolution of the spot areas within the active longitudes indicates a stellar activity cycle, during which one active longitude dominates the stellar activity, to be about 6.5 years. Then, a total cycle, comprising two consecutive periods of activity of both active longitudes, is about 13 years. In 1999, the activity switched to the other active longitude. This declared the beginning of a new (half-) cycle. based on observations collected at the Nordic Optical Telescope (NOT), La Palma, Spain; the 2.6 m and 1.25 m telescopes of the Crimean Astrophysical Observatory, Ukraine; the 2m telescope of the National Astronomical Observatory, Rozhen, Bulgaria.

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