1999/12/08 by A. Latorre, D. Montes, Latorre, A. +4
Physics and Astronomy · #Astronomy and Astrophysical Research #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/9912160
Latex file with 6 pages, 5 figures. Also available at http://www.ucm.es/info/Astrof/pub_dmg.html#cs11_bflyn to be published in ASP Conf. Ser., The 11th Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun, (October 4th - 8th, 1999, Puerto de la Cruz, Tenerife, Spain), R. Garcia Lopez, R. Rebolo, M.R. Zapatero Osorio (eds.)
arxiv created 1999/12/08 · openalex publication_date 1999/12/08 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
We have analysed several multiwavelength optical observations (Halpha, Hbeta, Hepsilon, Ca II H & K, Ca II IRT lines) of chromospherically active binary system OU Gem, taken in three observation runs: March 1996, April 1998 (using the SOFIN spectrograph and the Nordic Optical Telescope) and January 1999 (using the ESA-MUSICOS spectrograph and the Isaac Newton Telescope). The spectra show double Halpha and Hbeta absorption lines, but after applying the spectral subtraction technique, clear excess emission is seen in both components. The two stars have the Ca II IRT lines in emission, strong emission in the Ca II H & K lines and small emission in the Hepsilon line. Although they have very similar spectral types, the cool one is more active than the hot one in all runs, except for MUSICOS run, and in all spectral lines, except for Ca II IRT lines.