COMMISSION 27 OF THE I. A. U.
        INFORMATION BULLETIN ON VARIABLE STARS
                    Number 1568

                                Konkoly Observatory
                                Budapest
                                1979 March 14




    PERIODS AND LIGHT CURVES OF THE ECLIPSING BINARIES
            BV ERIDANI AND BW ERIDANI


Since their discovery by Hoffmeister (1933, 1936), the eclipsing binaries
BV and BW Eri have experienced little attention. Solov'yov (1954 a, b)
published a few minima from plates of the Stalinabad sky patrol.
Photoelectric observations by Baade in 1976 and by Duerbeck in 1977
furnished complete light curves. The derived periods were improved by
the use of photographic minima from Bamberg sky patrol plates, and by
Solov'yov's early minima:


BV Eri: J.D. hel. (primary min.) = 2 443 449.7193 + 0.5076643 * E

BW Eri: J.D. hel. (primary min.) = 2 443 448.6840 + 0.6384773 * E


BV Eri is an EB system with a remarkably short period. The colour of the
system corresponds to spectral type F2 V. The light curve shows an annular
primary minimum and a total secondary minimum.
BW Eri is also an EB system. The colour corresponds to spectral type A3 V.
The primary minimum is annular, the secondary is total.
Both light curves (in UBV) are shown in Figs. 1 and 2. A thorough investigation
and an analysis of the light curves will be published later.

Acknowledgements. D.B. was a visiting astronomer at the Cerro Tololo Inter-
American Observatory, which is operated by the Association of Universities
for Research in Astronomy, Inc., under contract with the National Science
Foundation. D.B. and H.W.D. were also visiting astronomers at the European
Southern Observatory, La Silla. H.W.D. and M.T.K. thank Professor J. Rahe
for the opportunity to use the Bamberg plate collection and for the hospitality
during their stay at the Bamberg Observatory.


                       [FIGURE 1]

  Fig. 1. (From above): U B V light curves of BV Eri, relative to SAO 149230.
  The scale is given for the B magnitudes; the U magnitudes are shifted
  by +0.3m, the V magnitudes by -0.3m.

                       [FIGURE 2]

  Fig. 2. (From above): U B V light curves of BW Eri, relative to SAO 169137.
  The scale is given for the B magnitudes; the U magnitudes are shifted
  by +0.3m, the V magnitudes by -0.3m.




                   D. BAADE
                   Astronomisches Institut der Universitat
                   Steinfurter Strasse 107
                   4400 Munster, F.R.G.

                   H. W. DUERBECK and M. T. KARIMIE *
                   Observatorium Hoher List
                   der Universitats-Sternwarte Bonn
                   5558 Daun, F.R.G.

                   * Stipendiat der Humboldt-Stiftung,
                    Bonn-Bad Godesberg, F.R.G.





References:

Hoffmeister, C. 1933, Astr. Nachr. 247, 281. [BIBCODE 1933AN....247..281H ]
Hoffmeister, C. 1936, Astr. Nachr. 258, 39. [BIBCODE 1936AN....258...39H ]
Solov'yov, A. 1954a, Astr. Tsirk. 149.
Solov'yov, A. 1954b, Astr. Tsirk. 151.