Apsidal motion and TESS light curves of three southern close eccentric eclipsing binaries: GM Nor, V397 Pup, and PT Vel
New ground-based and space-based photometric data have been obtained and archival spectroscopic measurements were used in this study of three detached early-type and southern-hemisphere eccentric eclipsing binaries GM Nor (P = 1.88 d, e = 0.05), V397 Pup (3.00, 0.30), and PT Vel (1.80, 0.12). Their...
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Main Authors | , , , , , , , , , , , , |
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Format | Journal Article |
Language | English |
Published |
13.08.2024
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Subjects | |
Online Access | Get full text |
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Summary: | New ground-based and space-based photometric data have been obtained and
archival spectroscopic measurements were used in this study of three detached
early-type and southern-hemisphere eccentric eclipsing binaries GM Nor (P =
1.88 d, e = 0.05), V397 Pup (3.00, 0.30), and PT Vel (1.80, 0.12). Their TESS
observations in several sectors have also been included and the corresponding
light curves were solved using the Phoebe code. As a result, new accurate
photoelectric times of minimum light have been obtained. 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 for the
elements of apsidal motion were obtained. Using ESO archive spectroscopy, for
V397 Pup, the precise absolute parameters were newly derived: M1 = 3.076(35)
M$\odot$, M2 = 2.306(35) M$\odot$, and R1 = 2.711(55) R$\odot$, R2 = 1.680(55)
R$\odot$. For PT Vel the absolute dimensions were improved: M1 = 2.204(25)
M$\odot$, M2 = 1.638(25) M$\odot$, and R1 = 2.108(30) R$\odot$, R2 = 1.605(30)
R$\odot$. For GM Nor, the less accurate absolute parameters based on the light
curve analysis were evaluated: M1 = 1.94(15) M$\odot$, M2 = 1.84(14) M$\odot$,
and R1 = 2.27(20) R$\odot$, R2 = 2.25(20) R$\odot$. We found more precise and
relatively short periods of apsidal motion of about 80, 335, and 160 years,
along with the corresponding internal structure constants, log k2, -2.524,
-2.361, and -2.563, for GM Nor, V397 Pup, and PT Vel, respectively.
Relativistic effects are small but not negligible, making up to 10\% of the
total apsidal motion rate in all systems. No marks of the presence of the third
body were revealed in the light curves, on the O-C diagrams, or in the reduced
spectra of the eccentric systems studied here. |
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DOI: | 10.48550/arxiv.2408.06910 |