COMMISSION 27 OF THE I.A.U.
                INFORMATION BULLETIN ON VARIABLE STARS
                            Number 3275

                                                        Konkoly Observatory
                                                        Budapest
                                                        22 December 1988

                                                        HU ISSN 0374 - 0676


                 A NEW VARIABLE STAR BD +2d1867

During the observations of the eclipsing binary YY CMi, the star
BD +2d1867, which served as a comparison star, turned out to be variable. No
information about the variability of this star can be found in literature
or in the Center of the Star Data in Strasbourg.
   During the present and the previous observational seasons photoelectric
observations of the new variable were performed in order to determine its
variability type. The observations were carried out at the Astronomical
Observatory of the Jagiellonian University in Cracow using the 50 cm Cassegrain 
telescope, as well as the mountain station Roztoki Gorne using a 20cm
refractor. Differential measurements of the star were made with a V filter
using BD +1d1994 as the comparison star. The light constancy of the comparison
star was checked against BD +1d1989. The observations were corrected for
atmospheric extinction using mean extinction coefficients for each observation
site. A detailed description of both photometers and photometric systems was
published by Flin et al. (1986). Data concerning the three stars mentioned
above are given in Table I.

                         Table I

               Data about the stars involved

star              BD       HD      ptm   ptg   Sp

new variable   +2d1867    66853    9.1m  9.4m  F2
comparison     +1d1994    67028    8.2   8.3   A2
check          +1d1989    66829    9.1   9.4   F

   The new variable star usually changes its brightness with an amplitude
of about 0.1 within a period of about 3 hours. There were also nights when
the star kept a nearly constant brightness. The light changes over six nights
with the largest number of observations are presented in Figure 1. Time
is expressed in fractions of a day and the brightness is given as the
difference between the comparison and the variable star expressed in stellar
magnitudes with zero point corresponding to the mean value for all differences 
(341 observational points).


                             [FIGURE 1]


   14 times of maxima were determined and the tentative elements for the new
variable were estimated:

Moment of maximum HJD = 2446768.6343+ 0.1194660d E
                            +/-.0034       +/-8

   The times of maxima and the O-C calculated from the above formula are
given in Table II.


                            Table II

HJD 24...        E        O-C        HJD 24..       E       O-C

45673.4835    -9167    -0.0057       46826.4703    484     0.0145
46082.4334    -5744     0.0120       46827.3923    492    -0.0192
46082.5411    -5743     0.0002       46851.4364    693     0.0122
46137.3662    -5284    -0.0096       46857.3970    743    -0.0005
46506.2970    -2196     0.0100       47176.3614   3413    -0.0104
46506.4058    -2195    -0.0005       47176.4728   3414    -0.0184

   Taking into account the spectral type of the new variable and the amplitude 
changes, the authors suggest BD +2d1867 to be a Delta Sct-type variable.
   It would be advantageous to obtain as many observations as possible
during one night. This is difficult at our Observatory because of its high
latitude. For this reason observations made at lower latitudes are highly
desirable.
   This work was partially supported by the grant RPBR-I-11-1 from Polish
Ministry of National Education.


                    M. KURPINSKA-WINIARSKA
                         M. WINIARSKI
                          ST. ZOLA

                    Astronomical Observatory
                 of the Jagiellonian University
               ul. Orla 171, 30-244 Krakow, Poland



Reference:

Flin, P., Winiarski, M., Zola, St., 1986, I.B.V.S. 2678.