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

Bibcode
2005MNRAS.356.1362D
DOI
10.1111/j.1365-2966.2004.08571.x
Davis, J.; Mendez, A.; Seneta, E. B.; Tango, W. J.; Booth, A. J.; O'Byrne, J. W.; Thorvaldson, E. D.; Ausseloos, M.; Aerts, C.; Uytterhoeven, K.
Referencia bibliográfica

Monthly Notices of the Royal Astronomical Society, Volume 356, Issue 4, pp. 1362-1370.

Fecha de publicación:
2
2005
Revista
Monthly Notices of the Royal Astronomical Society
Número de autores
10
Número de autores del IAC
0
Número de citas
29
Número de citas referidas
19
Descripción
The bright southern binary star β Centauri (HR5267) 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 442nm 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 +/- 0.07d, semimajor axis 25.30 +/- 0.19mas, inclination 67.4 +/-0.3, eccentricity 0.821 +/- 0.003, distance 102.3 +/- 1.7pc, primary and secondary masses M1=M2= 9.1 +/- 0.3 Msolar and absolute visual magnitudes of the primary and secondary M1V=-3.85 +/- 0.05 and M2V=-3.70 +/- 0.05, respectively. The high degree of accuracy of the results offers a fruitful starting point for future asteroseismic modelling of the pulsating binary components.
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Con árbitro
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