COMMISSIONS 27 AND 42 OF THE IAU
              INFORMATION BULLETIN ON VARIABLE STARS
                           Number 4076

                                                 Konkoly Observatory
                                                 Budapest
                                                 25 August 1994

                                                 HU ISSN 0374 - 0676


             NEW LIGHT CURVES AND PERIOD OF BV ERIDANI


 The eclipsing binary system BV Eri was discovered by Hoffmeister (1933). In 1954
Solov'yov published two minimum times of BV Eri. The system was observed photometrically 
by Baade and Duerbeck (1979) in 1976 and 1977, in 1983 they reported an analysis
of the spectroscopic orbit and the light curves.
 The present work was carried out with a single channel photoelectric photometer 
attached to 35 cm reflecting telescope in BV bands at Yunnan Observatory from October
to December 1984. The star SAO 149195 and SAO 149230 was used as the comparison
and check star, respectively. From our observations we obtained 598 points in B band
and 596 points in V band, in the meantime two primary minimum times and secondary a
secondary minimum time was derived, which are listed in the following Table. All 
observational data have been corrected for atmospheric extinction and reduced to the standard
UBV system. The light curves are displayed in Figures 1 and 2.

 We have collected all minimum times that we could find and calculated new light
elements by means of the least-squares method:

           Min.I=JD(Hel.)2443449.7320+0.5076669d x E
                                +/-66     +/-10

                          Table 1

JD(Hel.)         E          (O-C)     Weight  Source
2431052.2700   -24420.5    0.0174        1   Solov'yov
2431180.4900   -24168      0.0515        1   Solov'yov
2439059.4653    -8648      0.0366        1   Bamberg
2439767.5632    -7253     -0.0608        1   Bamberg
2440592.1167    -5629      0.0416        1   Bamberg
2441619.0528    -3606     -0.0324        1   Bamberg
2441620.0431    -3604     -0.0574        I   Bamberg
2442011.9910    -2832     -0.0284        1   Bamberg
2442013.9826    -2828     -0.0674        1   Bamberg
2443449.7207        0     -0.0113       10   Baade et al.
2444892.4762     2842     -0.0451        1   Baade et al.
2446032.2424     5087      0.0089       10   This paper
2446034.2726     5091      0.0084       10   This paper
2446048.2335     5118.5    0.0085       10   This paper


                          [FIGURE 1]

         Figure 1. The light curve of BV Eri in B band.

                          [FIGURE 2]

         Figure 2. The light curve of BV Eri in V band.

                          [FIGURE 3]

                  Figure 3. The O-C diagram


  In calculation we assigned weight 1 to the photographic and spectroscopic minimum
times, weight 10 to the photoelectric minimum times (see Table 1). Using the O-C
residuals listed in Table 1 we plotted the O-C diagram (Figure 3) in which the symbol
"+" means the photographic and spectroscopic minimum times and the symbol "o" means
the photoelectric minimum times. In this O-C diagram the scatter is very high and
no systematic trend appears. The light curve analysis using Wilson-Devinney synthesis
method will be published elsewhere.


                        Gu SHENGHONG
                        Liu QINGYAO
                        Yang YULAN
                        Zhang ZHOUSHENG
                        Yunnan Observatory
                        Academia Sinica
                        Kunming
                        China


References:

Baade, D., Duerbeck, H. W. and Karimie, M. T., 1979, IBVS, No. 1568
Baade, D., Duerbeck, H. W., Karimie, M. T. and Yamasaki, A., 1983, Astrophys. Space
   Sci., 93, 69 [BIBCODE 1983Ap&SS..93...69B ]
Hoffmeister, C., 1933, Astron. Nachr., 247, 281 [BIBCODE 1933AN....247..281H ]
Solov'yov, A. V., 1954, Astron. Tsirk., 149, 20