Abstract:
In this study we performed the first detailed photometric and period analysis of the
recently discovered eclipsing binary star V2783 Ori. The analysis of the
light curve has shown that the system is in a detached configuration, with
the orbital eccentricity e = 0.274 ± 0.008. The
photometric mass ratio of V2783 Ori determined from the light curve analysis
is q = 0.734 ± 0.015. The absolute parameters of
the system were obtained as a result of the light curve solution. Absolute
parameters were found as follows: masses
M1 = 1.80 ± 0.01 M☉,
M2 = 1.32 ± 0.01 M☉,
radii
R1 = 2.19 ± 0.10 R☉,
R2 = 1.91 ± 0.10 R☉,
temperatures
T1 = 8325 ± 100 K and
T2 = 8300 ± 100 K.
A comparison of
these parameters with theoretical stellar models show that the secondary
component is located inside the main-sequence band and still close to ZAMS,
while the primary component is located in the middle of ZAMS-TAMS limits.
The distance of the system determined from the absolute parameters,
d = 1064 ± 150 pc, takes into account the interstellar
reddening.
The (O--C) diagram was discussed considering all
reliable minima times found in the literature and new values for the
parameters of the apsidal motion and light-time effect were found. The
apsidal motion rate of V2783 Ori is
dω/dt = 0.0063 ± 0.0017 deg cycle-1,
and it corresponds to an apsidal
motion period of U = 656 ± 103 yr. The third body
orbital period is 10 ± 2 yr, its minimal mass is 0.82 ± 0.11 M☉.
Full text version of this article in
PDF.
; Bulut, A.
