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Evidence for mass loss in visual binary stars
Astrophysics and Space Science, 1988The present status of the observational evidence about mass loss in visual binary and multiple systems is reviewed. Particular emphasis is placed on the importance of mass-loss rates measures in these stars, as a systematic study would provide useful constraints in two fields. First, as mass-outflows processes are not modified by the interaction of the
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Visual binaries among the barium stars. II - HD 105902
Publications of the Astronomical Society of the Pacific, 1977Photometric and spectroscopic observations are presented of both members of the binary star system HD 105902 (ADS 8448) whose primary component is a barium star of spectral class K5 Ba 2. The visual absolute magnitude for the barium star primary is found to be +2.7 and the distance to the system is 190 pc.
R. B. Culver, O. G. Franz, P. A. Ianna
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Evaluation of Binary Star Formation Models Using Well-Observed Visual Binaries
2019Creation of the Galaxy model describing formation and evolution of binary stars requires generating and testing hypotheses related to the process of formation of binary stars and distributions of their characteristics. A set of hypotheses can be generated on the basis of a number of publications that suggested the formation of binary systems.
Oleg Malkov +8 more
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Orbit of the visual binary star 61 Cyg
Astronomische NachrichtenAbstractWe present the orbit and the mass estimates for the components of the visual binary star 61 Cyg obtained with the positional observations, including the high‐precision Gaia data, and the measurements of differences in the radial velocities and the radial accelerations of the components.
I. S. Izmailov, A. A. Apetyan
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Improved orbit for the visual-binary star 40/41 Dra
Astrophysics, 2012Families of orbits of the visual binary star 40/41 Dra (ADS 11061), a near-polar visual binary star (αJ2000 =18h00m; δJ2000; δJ2000 = +80°00′ ) which is a wide pair in the neighborhood of the sun ( πt = 19mas ), are calculated. Both components are spectrally binary and belong to the late spectral classes K2V and F7.
A. A. Afanasyeva, E. A. Grosheva
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The Orbital Elements of a Visual Binary Star
2006Although astronomers regard the brighter component as fixed and map the motion of the fainter one around it, in reality, both stars in a binary system move in ellipses around the common centre of gravity. The size of the ellipse is inversely proportional to the mass of the star, so in the Sirius system, for instance, the primary has a mass of 2.1 sun ...
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Kinematics and Physics of Celestial Bodies, 2009
Eclipsing variables in visual binary and multiple stars are searched using data from GCVS, WDS, and CCDM catalogs. The list of 421 eclipsing variables is obtained. The masses of components of multiple systems from the list are estimated using the mass-luminosity relation for the main sequence stars.
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Eclipsing variables in visual binary and multiple stars are searched using data from GCVS, WDS, and CCDM catalogs. The list of 421 eclipsing variables is obtained. The masses of components of multiple systems from the list are estimated using the mass-luminosity relation for the main sequence stars.
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Probing the interior physics of stars through asteroseismology
Reviews of Modern Physics, 2021Conny Aerts
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