Spectroscopic binary stars and the CHARA array

2003 ◽  
Author(s):  
Harold A. McAlister ◽  
Theo A. ten Brummelaar ◽  
William G. Bagnuolo, Jr. ◽  
David H. Berger ◽  
Thomas Fallon ◽  
...  
Keyword(s):  
Binary Stars ◽  
Spectroscopic Binary ◽  
Chara Array

scholarly journals Long Baseline Interferometry and Binary Stars

1983 ◽  
Vol 62 ◽  
pp. 191-201
Author(s):  
John Davis
Keyword(s):  
Binary Stars ◽  
Binary Systems ◽  
Current Status ◽  
Fundamental Properties ◽  
Long Baseline ◽  
Stellar Interferometer ◽  
Spectroscopic Binary ◽  
Future Plans ◽  
Intensity Interferometer

AbstractThe observations of α Vir with the Narrabri Stellar Intensity Interferometer demonstrated the potential of long baseline interferometry for the determination of fundamental properties of double-lined spectroscopic binary systems. Since the completion of the programme with the Narrabri instrument the Chatterton Astronomy Department has been conducting a study aimed at developing a stellar interferometer with limiting magnitude V ≳ +8 and maximum baseline ≳ 1 km (resolution at 500 nm ≲ 7 × 10−5 seconds of arc). The way in which a long baseline interferometer may be used in the study of binary stars is outlined, the requirements for this work are discussed, and the current status and future plans of the Chatterton Astronomy Department’s programme to develop a new long baseline interferometer are summarised.

scholarly journals On the Distribution of Young Spectroscopic Binary Stars Over the Major Semiaxes of their Orbits

1982 ◽  
Vol 69 ◽  
pp. 129-131
Author(s):  
E.I. Popova ◽  
A.V. Tutukov ◽  
B.M. Shustov ◽  
L.R. Yungelson
Keyword(s):  
Binary Stars ◽  
Binary Systems ◽  
Spectroscopic Binaries ◽  
Close Binary ◽  
Physical Parameters ◽  
Origin And Evolution ◽  
Spectroscopic Binary ◽  
Visible Spectra ◽  
Major Semiaxes ◽  
The Masses

About 60% of stars of the disc population in our Galaxy are close binary systems (CBS). Half of the known CBS are spectroscopic binary stars (Kraitcheva et al., 1978).To know the distribution of a correlation between the masses of CBS components and semiaxes of their orbits is necessary for the investigation of the origin and evolution of CBS. For such statistical investigations, a catalogue of CBS was compiled at the Astronomical Council. The catalogue is based on the 6th Batten catalogue (Batten, 1967), its extensions (Pedoussant and Ginestet, 1971; Pedoussant and Carquillat, 1973) and data published up to the end of 1980 (Popova et al., 1981). Now it is recorded on magnetic tape and contains data on 1041 spectroscopic binaries; 333 of them are stars with two visible spectra. The latter are mostly systems prior to mass exchange and the distribution of physical parameters in these systems reflects the distribution and presumably conditions at the time of formation. Using some assumptions, we can obtain for spectroscopic binaries masses of the components M1 and M2 (or the ratio q = M1/M2) and semiaxes of their orbits. Masses of components with the known sin i were obtained by the usual technique; when sin i was not known, masses were estimated from the spectra. We shall discuss here the distribution of CBS in the M-a plane.

scholarly journals Speckle Observations of Triple Stars

1992 ◽  
Vol 135 ◽  
pp. 555-557
Author(s):  
Syuzo Isobe ◽  
Naoshi Baba
Keyword(s):  
Binary Stars ◽  
Angular Resolution ◽  
Ccd Camera ◽  
Aging Effect ◽  
Diffraction Limit ◽  
Visual Binary ◽  
San Pedro ◽  
Spectroscopic Binary ◽  
Visual Binary Stars ◽  
Triple Stars

Our speckle observations were started in 1987 using a 212-cm telescope at San Pedro Martir Observatory in Mexico. A D-IMOSS camera was used until 1990 and an I-CCD camera was introduced in 1991. The old camera has only 0″.20 angular resolution because of an aging effect in its intensifier, while the new camera has 0″.06 angular resolution, which is nearly equal to the diffraction limit of the telescope. 128 visual binary stars and 755 spectroscopic binary stars have been observed. The numbers of stars and observations each year are shown in Table 1 and all the observed data are given in a series of papers by Isobe et al. (1990a, 1990b, 1992a) and Miura et al. (1992).

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