1999A&A...341..527E

We present new results from high-resolution spectroscopic observations of the late-type fast rotator BD+22 4409, revealing interesting aspects about its magnetic activity that have not been considered before. Analysis of the extremely variable and rotationally broadened chromospheric Hα emission profile provides clear evidence for an intense and continuous downflow of absorbing material. A high level of activity was also exhibited in the form of two consecutive flares that lasted for almost five hours. The decay of the second flare was accompanied by a dramatic absorption in the blue half of the Hα profile that is attributed to the development of cool flare loops. The observed circulation of material and the presence of magnetic loops in connection to the chromospheric flare suggest plasma is being effectively transferred between the chromosphere and the corona. As opposed to similar active and fast rotators, direct evidence of cool prominence clouds has not been found in this star. The results provide strong support for recent theoretical studies by van den Oord et al. (1997, A&A, submitted). In that work it was concluded that such prominences are only stable at some distance from the star in the equatorial plane. Unstable material would be expected to flow towards the poles along magnetic lines. The inclination of BD+22 4409, i∼50°, favours the detection of such flow as an asymmetry in chromospheric lines profiles. However, it could make clouds undetectable if they can never be seen in projection on the disk.