Apsidal motion and TESS light curves of two southern eclipsing binaries with high eccentricity: V1647 Sgr and V2283 Sgr
Annotatsiya
The study of apsidal motion rates in eccentric eclipsing binaries provides an important observational test of theoretical models of stellar structure and evolution. Precise physical parameters of the stellar components together with systematic measurements of the periastron advance are needed. We present new results of our long-term observational project to analyze the apsidal motion in early-type eccentric eclipsing binaries. New ground- and space-based photometric data were obtained, and archival spectroscopic measurements were used in this study of two detached southern hemisphere eclipsing binaries: V1647 Sgr ( P = 3 . d , e = 0.41), and V2283 Sgr (3 . d ,47, 0.49). Their TESS observations in four sectors were also included, and the corresponding light curves were solved using the code P HOEBE . The newly completed O − C diagrams were analyzed using all reliable timings found in the literature and calculated using the TESS light curves. New or improved values were obtained for the elements of apsidal motion. Using archival spectroscopy for V1647 Sgr, we improved the precise absolute parameters to M 1 = 2.184(0.035) M ⊙ , M 2 = 1.957(0.035) M ⊙ , and R 1 = 1.839(0.015) R ⊙ , R 2 = 1.716(0.015) R ⊙ . For V2283 Sgr, the absolute dimensions were newly estimated to M 1 = 2.178(0.10) M ⊙ , M 2 = 1.547(0.10) M ⊙ , and R 1 = 1.796(0.01) R ⊙ , R 2 = 1.544(0.01) R ⊙ . We improved relatively long periods of apsidal motion of about 580 and 530 years, together with the corresponding internal structure constants, log k 2 , –2.394, and –2.418, for V1647 Sgr and V2283 Sgr, respectively. The relativistic contribution to apsidal motion is not negligible. It is about 12 and 14% of the total rate of apsidal motion for V1647 Sgr and V2283 Sgr, respectively. No signs of an additional body were revealed in the light curves or in the O − C diagrams of the two eccentric systems.