Orbital parameters, masses and distance to β Centauri determined with the Sydney University Stellar Interferometer and high‐resolution spectroscopy

By J. Davis, A. Mendez, Eugene Seneta, W. Tango, A. Booth, J. O'Byrne, E. Thorvaldson, M. Ausseloos, C. Aerts, K. U. U. O. Sydney and 12 more. 2004

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The bright southern binary star β Centauri (HR 5267) has been observed with the Sydney University Stellar Interferometer (SUSI) and spectroscopically with the European Southern Observatory Coude Auxiliary Telescope and Swiss Euler telescope at La Silla. The interferometric observations have confirmed the binary nature of the primary component and have enabled the determination of the orbital parameters of the system. At the observing wavelength of 442 nm the two components of the primary system have a magnitude difference of 0.15 ± 0.02. The combination of interferometric and spectroscopic data gives the following results: orbital period 357.00 ± 0.07 d, semimajor axis 25.30 ± 0.19 mas, inclination 67. ◦ 4 ± 0. ◦ 3, eccentricity 0.821 ± 0.003, distance 102.3 ± 1.7 pc, primary and secondary masses M 1 = ( ◦ )( ◦ ) .

Subfields: Astronomy and Astrophysics, Geology

View Paper: https://www.semanticscholar.org/paper/24105d5fb801854b81c2b4925a988c64d8745ff9

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In Astronomy and Astrophysics

1. A. Moffat
2. W. Tango
3. J. North
4. R. Kuschnig
5. J. Davis
6. S. Rucinski
7. P. Tuthill

Citations in the corpus

• Massive pulsating stars observed by BRITE-Constellation - I. The triple system β Centauri (Agena) (2016, methodology): “It appeared, however, that for the SUSI observations (Davis et al. 2005) times translated from the original mean MJDs are late by about 3.5 d in the 4th Catalog of Interferometric Measurements.”
• γ2 Velorum: orbital solution and fundamental parameter determination with SUSI (2007, background): “It has been shown that the dynamical parallax of some binary stars can be significantly different to the Hipparcos parallax (Davis et al. 2005; Tango et al. 2006).”