Name/Affiliation: Lalitha Sairam (Tata Institute of Fundamental Research)
Spectroscopic characterisation of tidally interacting binaries
The RS CVn binaries are the class of system typically composed of a chromospherically G- or K-type stars with a late-type subgiant or main-sequence companion. They are tidally locked close binaries, they are also fast rotators. In this talk, I will present our ongoing work in the context of systematic study of coronal X-ray emission from a young pre-main-sequence RS Cvn system--HD 155555. This system is composed of a G5 IV primary and a K0 IV secondary and has an orbital period of 1.68 d. We reconstruct the emission measure distribution (EMD(T)) using spectral line analysis and consequently obtain the elemental abundance from EMD(T). Furthermore, we investigate the line broadening by analysing the strong line profiles. In order to provide a better insight into the line broadening we also carried out a comparative study between HD 155555, BY Dra binaries and Algol.