Properties and nature of Be stars XXIII. Long-term variations and physical properties of kappa Dra

We present an analysis of new spectroscopic observations of the bright Be star kappa Dra obtained at the Ondrejov observatory during 1992 - 2003 and UBV photometric observations secured at several observatories. The fundamental stellar parameters have been obtained from a comparison with a grid of NLTE model atmospheres. The best fit was found for Teff=14000K, log g = 3.5, and v sin i = 170km/s. These values together with a Hipparcos parallax lead to a stellar mass M=4.8+-0.8 M_solar and radius R=6.4+-0.5 R_solar. Long-term variations of kappa Dra were analysed using measurements of equivalent widths, central intensities, peak intensities of emission lines and emission peak velocity differences for H-alpha, H-beta, H-gamma, H-delta, and some helium, silicon, and iron lines. It turned out that the previously reported period of 23 years in the variation of the emission strength is probably a cyclic, not a strictly periodic phenomenon. An attempt to find out a period from all available records of the H-beta emission strength led to a value of 8044+-167 days (22.0 years) but the phase plots show that each cycle has a different shape and length. For the moment, the nature and origin of the disk around kappa Dra still remains unknown. From the comparison of the electronic spectra obtained at different phases of the long-term cycle and synthetic spectra it appears that there are no detectable changes in the photospheric part of the Balmer lines related to variations in the Balmer emission strength which could be attributed to an extended photosphere corresponding to inner parts of the disk, optically thick in continuum.