A study of the time variability and line profile variations of κdra

Abstract

We present a spectroscopic analysis of the bright Be star κ Dra. Two independent sets of radial velocity (RV) measurements were obtained by direct measurement and using a line profile disentangling technique. By combining solutions from codes FOTEL and KOREL, we derived improved orbital elements. From the RVs of the Balmer lines and also from some strong metallic lines we found that all RV variations are phase-locked with the orbital period. V /R variations were obtained for Hα, Hβ, Hγ and some other photospheric lines. A moving absorption bump superposed over the emission line profiles was detected. The orbital solutions for κ Dra were derived assuming a circular orbit with a period P = 61d.5549 and K = 6.81 km s-1. We failed to find absorption or emission lines for the unresolved secondary component.