Photospheric and chromospheric active regions on three single-lined RS CVn binaries
Department of Physics and Astronomy, University of Catania, via S. Sofia 78, 95123 Catania, Italy e-mail: firstname.lastname@example.org
2 INAF - Catania Astrophysical Observatory, via S. Sofia 78, 95123 Catania, Italy
Accepted: 5 October 2005
A monitoring of three active RS CVn binaries has been performed with medium resolution spectroscopy with the aim of investigating the behavior of chromospheric and photospheric inhomogeneities. Surface temperature, as recovered from line-depth ratios (LDRs), allowed us to map the photospheric spots, while the Hα emission has been used as an indicator of chromospheric inhomogeneities. We have found that the rotational modulation of the Hα emission is always in anti-phase with the temperature wave, i.e. at the time of our observations active regions at chromospheric and photospheric levels are closely spatially associated in these active stars. The residual Hα profiles, obtained as the difference between the observed spectra and non-active templates, are well reproduced by a two Gaussian fitting. The broad emission component, responsible for the wide emission wings in near all the spectra, is often blue-shifted with respect to the center of the stellar disk. The narrow Hα emission displays a phase-dependent variation in all stars and is anti-correlated with the photospheric diagnostics, while the broad one displays no or little rotational modulation. We suggest that the broad emission component is mainly related to physical phenomena, like micro-flaring or strong chromospheric velocity fields, occurring all over the star disk, while the central narrow emission is more affected by chromospheric plages. We have also detected a modulation of the intensity of the D3 line with the star rotation, suggesting surface features also in the upper chromosphere of these stars.
Key words: stars: activity / stars: starspots / stars: individual: VY Ari / stars: individual: HK Lac / stars: individual: IM Peg / techniques: spectroscopic / stars: binaries: close
© ESO, 2006