COMMISSION 27 OF THE I. A. U.
         INFORMATION BULLETIN ON VARIABLE STARS
                     Number 1942

                                   Konkoly Observatory
                                   Budapest
                                   1981 March 25

                                   HU ISSN 0374-0676



              REMARKS ON 6 VARIABLE STARS


EP And

Elements for this star have been announced by Locher, K.
(BBSAG Bull. 25) and the authors of the GCVS-Supplement 1976.
Sky-Patrol plates of the Hartha and Sonneberg Observatories
have been used to check the period in the years 1928-1976.
Improved elements
a) for the interval from J.D. 2425500-2437600:

    Min.(hel.)= J.D. 2427483.258 + 0.4041081d E      (EW)

b) for the interval from J.D. 2437600-2443000:

    Min.(hel.)= J.D. 2440152.449 + 0.4041070d E      (EW)


V 466 Cyg


In SAC 50 (1979) corrected elements for this Algol-type binary
were given to satisfy two minima of Diethelm, R. (Orion 120 and
126)
Twenty newly observed Min. I and II from 1954-1979 confirm the
elements of the GCVS. A period change since 1935 is not probable.


EG Sgr


Although this star has been often observed we have no clearness
about its true period, moreover, following the GCVS the period
should be variable.
Photographic investigations of Sonneberg Sky-Patrol plates from
1929-1979 and an analysis of the former published minima having
lead to the acceptance of the long value (4.97d). There are no
symptoms for a period change in the last 50 years. A new revision 
of 64 minima: found from 1903-1980 yields the   following
somewhat improved elements:
	Min.(hel.)= J.D.2441830.517+ 4.9723590d E         (EA)
A final decision whether the period is 4.97d or 2.49d is still
outstanding.


CSV 5844


Lukatskaya, F.J. discovered this star (=BD + 63d17) and announced
it as a possible eclipsing binary (Astron. Circ. 216.13, 1960).
Investigations of this star on 344 plates were carried out. The
photometric behaviour is characterised by a normallight of
10.70m ph. irregular appearing minima (depth about 0.5 mag.,
duration 6-8 days). Therefore CSV 5844 seems to be a member of the
BO-Cep group (Isb).



SAO 077615


In I.B.V.S. No. 1556 Harris, A.W. has given two possible values
of the period of this bright W UMa type star. A revision of 232
Hartha Sky-Patrol plates (1958-1977) yields 13 new minima I and
II, representable by a period near Harris' second variant. Moreover, 
an abrupt period increase of 1.5 sec. in 1971 was detected.
Elements available from J.D. 2436540-2441300:

    Min.(hel.)= J.D. 2436637.340 + 0.3464380d E        (EW)

and from J.D. 2441300-2443200:

    Min.(hel.)= J.D. 2441329.510 + 0.3464551d E        (EW)
            (8.9m-9.3m/9.3m ph.)



Huruhata's object in CMi


Huruhata announced a new bright Algol-type variable in I.B.V.S.
No. 1574.
From investigations of 200 plates he derived first elements
which could be confirmed on principle by further minima found
on 394 Sonneberg Sky-Patrol plates from 1942-1979.
The improved elements are:

     Min.(hel.)= J.D. 2444169.571 + 1.1806866d E      (EA)
             (10.85m-11.60m ph., no secondary minimum
                    D = 0.18p)





                           THOMAS BERTHOLD
                      Bruno-H.-Burgel-Sternwarte
                           DDR 7302 Hartha