Differential rotation of the active G5 V star κ 1 ceti: Photometry from the MOST satellite

Slavek M. Rucinski, Gordon A.H. Walker, Jaymie M. Matthews, Rainer Kuschnig, Evgenya Shkolnik, Sergey Marchenko, David A. Bohlender, D. B. Guenther, Anthony F.J. Moffat, Dimitar Sasselov, Werner W. Weiss

Research output: Contribution to journalArticlepeer-review

36 Scopus citations


About 30.5 days of nearly uninterrupted broadband photometry of the solar-type star κ 1 Ceti, obtained with the MOST (Microvariability and Oscillations of Stars) satellite, shows evidence for two large starspots with different rotation periods of 8.9 and ∼9.3 days (ΔΩ/Ω ≃ 4%). Ground-based measurements of Ca II H and K emission in 2002 and 2003 reveal variations in chromospheric activity with a period of about 9.3 days. The data were obtained during the MOST commissioning phase. When the data are combined with historical observations, they indicate that the 9.3 day spot has been stable in its period for over 30 yr. The photometry, with a sampling rate of approximately once per minute, was also used to search for acoustic (p-mode) oscillations in the star. We detect no clear evidence for p-modes in the κ 1 Ceti photometry, with a noise level around 7-9 μmag at frequencies in the range of 0.5-4 mHz (3 σ detection limit of 21-27 μmag). There were no flares or planetary transits during 30.5 days of MOST monitoring with light amplitudes greater than 2 mmag (durations >200 minutes) and 3 mmag (2-200 minute durations). While this rules out any close-in planets with Jupiter diameters ≥0.5 and orbital inclinations close to 90°, the scatter in differential radial velocities permit a close giant planet in a more highly inclined orbit.

Original languageEnglish (US)
Pages (from-to)1093-1104
Number of pages12
JournalPublications of the Astronomical Society of the Pacific
Issue number826
StatePublished - Dec 2004
Externally publishedYes

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science


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