1 Introduction

The variability of V382 Cygni was discovered by Morgenroth (1935). The eclipsing character of the system was suggested photographically by Petrov (1946). Petrov noted that the light curve is $\beta$ Lyrae type and the depths of the minima are nearly equal. The photographic light curve of Petrov was analyzed by Albo (1958). Pearce (1952) published the spectroscopic elements of the system and considered the spectral types of the components as O6.5 and O7.5. He found that the orbital velocities are exceedingly large ($K1+K2=710~{\rm~km \,s^{-1}}$). He also derived the masses of the components as $37.3 \,{M_\odot}$ and $32.7 {\, M_\odot}$ and the length of the semi-major axis of the relative orbit $(a\,\sin i)$ as $26.4 {\, R_\odot}$. Photoelectric UBV light curves of the system were obtained by Landolt (1964, 1975). Landolt's (1964) light curves were analyzed by himself using the Russell-Merrill Method. Landolt's (1975) light curves were analyzed using Wood's WINK method by Cester et al. (1978) and using the Wilson-Devinney method by Devinney & Twigg (1974). According to Cester et al., the system is not a detached but a contact binary. They gave the masses of the components as $38 {\, M_\odot}$ and $33.3 {\, M_\odot}$ (q=0.88). Koch et al. (1979) have obtained the IUE spectrum of V382 Cygni. The period variation of the system was studied by Mayer (1980, 1987), and Mayer et al. (1991). Popper & Hill (1991) analyzed the spectroscopic observations of Popper (1978) and obtained orbital solutions. They also obtained the absolute elements of the system. Popper & Hill gave the masses of the components as $32.6 {\, M_\odot}$ and $22.9 {\, M_\odot}$ (q=0.70). Popper (1980) lists the spectral types for V382 Cyg as O7.3V and O7.7V.

A recent spectroscopic investigation of the system was published by Harries et al. (1997). They also solved Landolt's (1975) light curves using the LIGHT2 method. They found that V382 Cygni is a contact system with masses of the components as $26 {\, M_\odot}$ and $19.3 {\,M_\odot}$ (q=0.74). These values of the masses are significantly lower than the previous ones. We decided to observe the system to obtain complete photoelectric light curves and reliable photometric solutions of V382 Cygni.