Masses of Astrometric Binaries

Details Masses of Astrometric Binaries Masses of Astrometric Binaries

Aug 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997esasp.402..417m&link_type=abstract

Proceedings of the ESA Symposium `Hipparcos - Venice '97', 13-16 May, Venice, Italy, ESA SP-402 (July 1997), p. 417-420

Astronomy and Astrophysics

Astronomy

2

Scientific paper

Among the double stars observed by Hipparcos and solved for their relative and absolute astrometry, the close pairs with an orbital period less than 10 years have a significant non-linear motion of their photocentre over the observation timespan. The amplitude of this motion is related to the size of the relative orbit of the two components and to the difference between the mass and intensity ratio. We present and discuss a specific treatment of the Hipparcos observations of the small sample of astrometric binaries with reliable ground-based orbital parameters. This leads to the determination of the mass ratio with an accuracy of about one per cent and of the masses of the individual components, the accuracy of which is ultimately linked to the quality of the parallax. Out of the 145 systems with ground-based orbits which were investigated in detail, 44 were solved for the scale of the photocentric orbit. For well-known systems, the masses derived from the Hipparcos data are compared to the values found in the literature.

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