V907 Sco Switched to the Eclipsing Mode Again

• Published in: The Astronomical journal Vol. 165; no. 3; pp. 81 - 92
• Main Authors: Zasche, Petr, Vokrouhlický, David, Barlow, Brad N., Mašek, Martin
• Format: Journal Article
• Language: English
• Published: Madison The American Astronomical Society 01-03-2023; IOP Publishing
• Subjects: Angular momentum; Astronomy; Binary stars; Eclipsing binary stars; Extrasolar planets; Inclination; Multiple stars; Parameters; Physical properties; Planet detection; Satellite observation; Satellites; Spectroscopic observation; Transit
• ISSN: 0004-6256; 1538-3881
• DOI: 10.3847/1538-3881/acae95

Abstract
V907 Scorpii is a unique triple system in which the inner binary component has been reported to have switched on and off eclipses several times in modern history. In spite of its peculiarity, observational data on this system are surprisingly scarce. Here we make use of the recent Transiting Exoplanet Survey Satellite observations, as well as our own photometric and spectroscopic data, to expand the overall data set and study the V907 Sco system in more detail. Our analysis provides both new and improved values for several of its fundamental parameters: (i) the masses of the stars in the eclipsing binary are 2.74 ± 0.02
M
⊙
and 2.56 ± 0.02
M
⊙
; and (ii) the third component is a solar-type star with mass
1.06
−
0.10
+
0.11
M
⊙
(90% C.L.), orbiting the binary on an elongated orbit with an eccentricity of 0.47 ± 0.02 and a period of 142.01 ± 0.05 days. The intermittent intervals of time when eclipses of the inner binary are switched on and off are caused by a mutual
26
.°
2
−
2.2
+
2.6
inclination of the inner- and outer-orbit planes, and a favorable inclination of about 71° of the total angular momentum of the system. The nodal precession period is
P
ν
=
63.5
−
2.6
+
3.3
yr. The inner binary will remain eclipsing for another ≃26 yr, offering an opportunity to significantly improve the parameters of the model. This is especially true during the next decade when the inner-orbit inclination will increase to nearly 90°. Further spectroscopic observations are also desirable, as they can help to improve constraints on the system’s orbital architecture and its physical parameters.