A photometric investigation of the eclipsing binary V505 Sagittarii

Details A photometric investigation of the eclipsing binary V505 Sagittarii A photometric investigation of the eclipsing binary V505 Sagittarii

Nov 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993aj....106.2058c&link_type=abstract

Astronomical Journal (ISSN 0004-6256), vol. 106, no. 5, p. 2058-2071

Astronomy and Astrophysics

Astronomy

13

A Stars, Astronomical Photometry, Eclipsing Binary Stars, F Stars, G Stars, Light Curve, Simplex Method, Triple Stars, Orbital Mechanics, Photoelectric Emission, Radial Velocity, Speckle Interferometry

Scientific paper

V505 Sgr is a classical Algol system consisting of an A2 V primary and a G5 IV secondary that fills its Roche lobe. New times of minimum light are presented. The period of the eclipsing system (1.18287d) varies, due in part to an orbital light-time effect. A third component has been detected that orbits the eclipsing pair. This investigation uses the SIMPLEX algorithm (Kallrath & Linnell, 1987) and the Differential Correction code (Wilson, 1979) to analyze two separate datasets. The results indicate the third component, an F8 V star, contirbutes about 5% of the light to the system. The minimum projected distance between the third component and the eclipsing pair is 37 AU. This implies an orbital period of about 105 years, a value that differs with the O-C data. The photometric solution, combined with recent spectroscopic data yields R1 = 2.14 solar radius and R2 = 2.24 solar radius and M1 = 2.20 solar mass and M2 = 1.15 solar mass.

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