COMMISSION 27 OF THE I.A.U.
               INFORMATION BULLETIN ON VARIABLE STARS
                            Number 1461

                                                      Konkoly Observatory
                                                      Budapest
                                                      1978 August 21


    ABOUT DISCOVERY OF THE 22.4-HR PERIODICITY IN THE
    VARIATIONS OF Halpha RADIAL VELOCITIES OF X PERSEI,
  THE OPTICAL COUNTERPANT OF THE X-RAY SOURCE 3U 0352+30

Radial velocity measurements of V and R components of Halpha
emission in the spectrum of X Persei, a peculiar B0e star have
been carried out to search for a periodicity analogous to the
existing 22 hr X-ray variations of 3U 0352+30.
   Two kinds of periodicity have been discovered. One of them
is with a period 22.4 hr. (amplitude K=15-17 km/sec) analogous to
22.4 hr. periodicity of the X-ray variations of the source
3U 0352+30. Another is with a 581-day one (amplitude K=35 km/sec)
(see Hutchings et al. 1974, Astrophys. J, 191, L101).
   Fig. 1 shows the phase dependences of Halpha radial velocities
(upper curve) and of V/R intensity ratio (lower curve), the 22.4
hr value has been adopted for the period.
   All these led us to the evident conclusion on the association 
of X Persei with the X-ray source 3U 0352+30.
   The X Per/3U 0352+30 system may be considered as a triple
system: a neutron star moving around a B0e primary with a period
of 22.4 hr., and this double system moving around a far third 
companion with a period 581 days.
   All the details on the spectral observation of the system
X Per/3U 0352+30 being carried out during the period November
1974 - March 1978 would be published in the Vol. 61 of Izv. Crim.
Obs.

                            T.S. GALKINA

                         Crimean Astrophysical
                             Observatory
                    p/o Nauchny, Crimea, 334413, USSR


                       [FIGURE 1]