COMMISSION 27 OF THE I. A. U.
              INFORMATION BULLETIN ON VARIABLE STARS
                           Number 3434

	                                       Konkoly Observatory
        	                               Budapest
                          	               20 February 1990

                                               HU ISSN 0374 - 0676


   A CCD LIGHT CURVE OF THE ECLIPSING CATACLYSMIC VARIABLE PG0027+260

  Ultraviolet extra object PG0027+260 (B=14.8) was reported by Green et
al. (1982) as cataclysmic variable candidate. Light curve evidence is necessary
to confirm it.
  The CCD light curve of PG0027+260 was observed in R color on 30 November, 
1989 with the 60/90/180 cm Schmidt telescope at Beijing Observatory,
using the BAO CCD light curve survey photometer system (Wei Mingzhi et
al. 1989). We chose two stars within the CCD field as comparison and check
stars respectively, denoted by C1 and C2. Figure 1 shows the light curves of
check star minus comparison and variable minus comparison. Each point in
the light curves is a one-hundred-second integration and the interval between
each integration is 12 seconds.
  The light curve shows definitely that PG0027+260 is an eclipsing cataclysmic 
binary system. The depth of primary minima is about 0.5 mag. Like
other cataclysmic variable system, the rapid changes in the brightness, which
is considered to be caused by mass transfer from the secondary, can be seen
in the light curve. The amplitude of rapid changes reach to 0.2 mag. The 
secondary minima is too weak to be distinguished from the strong rapid variations. 
This object is the second eclipsing cataclysmic variable confirmed by the
BAO Schmidt telescope CCD light curve survey photometer system, the other
one is PG0818+513(Chen Jiansheng et al. 1989).

  Two times of primary minima were obtained, they are:


                JD2447861.0689

                JD2447861.2154


The orbital period is about 0.146 d. We gave the ephemeris as follows,

           Min.I.=JD244 7861.06891 * 0.146 E

  The further observation and detailed study on physical model of this object
is in process.

                                  [FIGURE 1]

                                  Figure 1
CCD light curves in R color, upper is light curve of C2-C1, lower is that of
V-C1. Each point is a one-hundred-second integration, the interval between
each integration is 12 seconds. The uncertainty of each point is 0.01 mag.



                LI YONG, JIANG ZHAOJI, CHEN JIANSHENG, WEI MINGZHI
                       Beijing Astronomical Observatory
                         Chinese Academy of Sciences
                                 Beijing, China


 References:

Chen Jiansheng, Wei Mingzhi, and Liu Xiaowei, (1989) submitted to Act.
 Astron. Sin. [BIBCODE 1990AcASn..31..305C ]
Green, R. F., Ferguson, D. H., Liebert, J., and Schmidt, M., 1982, 
 P.A.S.P., 94 560 [BIBCODE 1982PASP...94..560G ]
Wei Mingzhi, Chen Jiansheng, and Jiang Zhaoji, (1989) submitted to P.A.S.P. [BIBCODE 1990PASP..102..698W ]