1997/09/18 by S. Randich, Sofia Randich, Randich, Sofia · 1 citation
Physics and Astronomy · #Astro and Planetary Science #Astrophysics (astro-ph) #Astrophysics and Star Formation Studies #FOS: Physical sciences #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/9709177
9 pages, LaTeX, 4 postscript figures. To appear in the proceedings of the 10th Cambridge Workshop on Cool Stars, Stellar, Systems and the Sun, eds. B. Donahue, J. Bookbinder
arxiv created 1997/09/18 · openalex publication_date 1997/09/18 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
A population of cool dwarfs with extreme rotational velocities (v sini > 100 km/sec) is present in young open clusters. ROSAT observations have shown that these very fast rotators exhibit a level of X-ray activity a factor of 3-5 below the saturated level which is usually observed (both in X-rays and other magnetic activity indicators) for `normally' fast rotators. This phenomenon has been denominated "Supersaturation". W UMa contact binaries seem to be supersaturated as well, while the scatter in the rotation-activity relation for RS CVn and BY Dra binaries does not allow us to clearly discern whether they exhibit supersaturation or not. Supersaturation is not seen in Halpha for Alpha Per supersaturated stars. Two alternative lines of interpretation are discussed.