Observations

DR Vul was observed photoelectrically at the Ege University Observatory on 40 nights during The 1993 and 1994 observing seasons. All observations were made with B and V filters which are very close to Johnson's standard system. BD 260 3827 and BD 260 3837 were used as comparison and check stars, respectively. The data related to the variable comparison and check stars are given in Table 1. During the observations, no significant light variation of the comparison and check star was found. The atmospheric extinction coefficients in each color for each observational night were calculated from the observations of the comparison star using conventional methods. Then, all the instrumental differential B and V

C. Qigek / Apsidal Motion Problem in the Eclipsing Binary Star DR Vulpeculae Table 1. The data for the observed stars.

Star

HD No.

a (2000)

5 (2000)

mu

Sp

DR Vul

339770

20" 13m.7

26° 45'.1

8m66

AO

Comparison

192043

20h 11-.9

26° 44'.1

7m.59

AO

Check

339764

20" 14m.4

27° 02'.9

9"\58

AO

Figure 1. The light and color curves of DR Vul in 1993.

magnitudes (in the sense of variable minus comparison) were corrected for atmospheric extinction and the light time effect of the Earth's motion. The instrumental differential B and V light and B-V color curves are shown in Figs 1 and 2.

The photometric phases in Figs 1 and 2 are calculated by using the following light elements given by Qifek, [10]:

HJD Min IJD = 2449162.4631(2) + 2d.2509350(15)E. (1)

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