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.

We report the results of spectral and photometric observations of DQ Her. Available spectra from International Ultraviolet Explorer (IUE), Hubble Space Telescope Faint Object Spectrograph (HST - FOS) and CCD photometry of one night were used. Some profiles revealing the variations of some spectral lines at different times are presented. There is variation with time for photometric observations and the brightness of DQ Her is changed from 14 mag. to 17.7 mag with clear display of burst. The ultraviolet luminosity for emitting region is in the range of (1.9x1031erg s−1). The mass accretion rate is in the range of (3.5x10−12M⊙yr−1). The line flux modulations at different times can be explained in terms of the accretion curtain model for intermediate polars, Kim & Beuermann (1996).

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