Photometric studies of BH Vir(
) were published by
Kitamura et al. (1957), Koch (1967), Hoffmann (1982),
Scaltriti (1988) and
Arevalo et al. (1987). These authors found large intrinsic
variations on BH Vir light curves on all phases. Hoffmann (1982) concluded
that these instrinsic variations were due to both components and suggested
that BH Vir should join the short-priod RS CVn group. Scaltriti et al.
(1985) attributed the activity to the primary star.
Zeilik et al. (1990)
and Zhai et al. (1990) made some starspot models to fit the light curves.
Since the variation of the light curve is very complicated, we selected
this system in our programme and made photometric observations.