V773 Cas, QS Aql, AND BR Ind: ECLIPSING BINARIES AS PARTS OF MULTIPLE SYSTEMS

Journal Article · Sun Jan 01 00:00:00 EST 2017 · Astronomical Journal (Online)

DOI:https://doi.org/10.3847/1538-3881/153/1/36· OSTI ID:22664044

Zasche, P.; Juryšek, J.; Nemravová, J.; Wolf, M.; Korčáková, D. ^[1]; Uhlař, R. ^[2]; Svoboda, P. ^[3]; Hoňková, K. ^[4]; Mašek, M.; Prouza, M. ^[5]; Čechura, J.

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1. Astronomical Institute, Charles University in Prague, Faculty of Mathematics and Physics, CZ-180 00, Praha 8, V Holešovičkách 2 (Czech Republic)
2. Private Observatory, Pohoří 71, CZ-254 01, Jílové u Prahy (Czech Republic)
3. Private Observatory, Výpustky 5, CZ-614 00, Brno (Czech Republic)
4. Variable Star and Exoplanet Section of Czech Astronomical Society, Vsetínská 941/78, CZ-757 01, Valašské Meziříčí (Czech Republic)
5. Institute of Physics, The Czech Academy of Sciences, Na Slovance 1999/2, CZ-182 21, Praha (Czech Republic)

Eclipsing binaries remain crucial objects for our understanding of the universe. In particular, those that are components of multiple systems can help us solve the problem of the formation of these systems. Analysis of the radial velocities together with the light curve produced for the first time precise physical parameters of the components of the multiple systems V773 Cas, QS Aql, and BR Ind. Their visual orbits were also analyzed, which resulted in slightly improved orbital elements. What is typical for all these systems is that their most dominant source is the third distant component. The system V773 Cas consists of two similar G1-2V stars revolving in a circular orbit and a more distant component of the A3V type. Additionally, the improved value of parallax was calculated to be 17.6 mas. Analysis of QS Aql resulted in the following: the inner eclipsing pair is composed of B6V and F1V stars, and the third component is of about the B6 spectral type. The outer orbit has high eccentricity of about 0.95, and observations near its upcoming periastron passage between the years 2038 and 2040 are of high importance. Also, the parallax of the system was derived to be about 2.89 mas, moving the star much closer to the Sun than originally assumed. The system BR Ind was found to be a quadruple star consisting of two eclipsing K dwarfs orbiting each other with a period of 1.786 days; the distant component is a single-lined spectroscopic binary with an orbital period of about 6 days. Both pairs are moving around each other on their 148 year orbit.

• OSTI ID: 22664044
• Journal Information: Astronomical Journal (Online), Vol. 153, Issue 1; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 1538-3881
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTROPHYSICS
COSMOLOGY AND ASTRONOMY
BINARY STARS
DIAGRAMS
DWARF STARS
ECLIPSE
ORBITS
RADIAL VELOCITY
SUN
SYSTEMS ANALYSIS
UNIVERSE
VISIBLE RADIATION