Magnetic activities on two single-lined RS Canum Venaticorum binaries IM Pegasi and $σ$ Geminorum

We present the study on continuous high-resolution spectroscopic observations of two long-period single-lined RS Canum Venaticorum (RS CVn) binary stars IM Pegasi (IM Peg) and $σ$ Geminorum ($σ$ Gem), obtained with the Hertzsprung SONG telescope during the 2015-2016 season. Chromospheric activity indicators H$_α$, Na I D$_{1}$, D$_{2}$ doublet, He I D$_{3}$, and H$_β$ lines have been analyzed by using the spectral subtraction technique. The expected chromospheric emission features in the H$_α$, Na I D$_{1}$, D$_{2}$ doublet, and H$_β$ lines confirm that both of two stars are very active systems. In the spectra, the He I D$_{3}$ line had been always detected in absorption feature. Although the behavior of chromospheric activity indicators is very similar for both stars, the activity level of IM Peg is much stronger than that of $σ$ Gem. Moreover, the EW variations of the H$_α$, He I D$_{3}$, and H$_β$ line subtractions correlate well and show different behavior among different orbital cycles, which indicates the presence and evolution of activity longitudes over the surface of two stars. Furthermore, the subtracted H$_α$ line profile is usually asymmetric. The red-shifted excess absorption features could be interpreted as a strong down-flow of cool absorbing material, while the blue-shifted emission component is probably caused by up-flow of hot materials through microflare events.

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