Orbital period of the symbiotic system AX Persei determined by the method of radial velocities

AX Persei belongs to a group of symbiotic stars, which are open binaries usually consisting of a cool giant and a white dwarf. The mass transfer between the components of these interacting systems is responsible for the manifestations of their observed outburst activity. In this article, we present the results of determining the orbital period of AX Persei based on the analysis of its radial velocity curve. We used 75 radial velocities, out of which 45 were collected from literature and 30 were derived using the spectra from ARAS database. Two methods were used to determine the radial velocities: the Doppler shift measurement of the sodium absorption doublet and the cross-correlation analysis. The result of the period analysis of the radial velocities of AX Persei is the orbital period of 681.2 ± 4.2days, which is in good agreement with the value determined by our previous analysis of photometric variability of the symbiotic system as well as with the values derived by other researchers.