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An Astrometric Study of the Low-Mass Binary Star Ross 614
Long accepted as the quintessential low-mass star, the secondary of thenearby diminutive astrometric binary Ross 614 has attracted considerableastrophysical interest. Unfortunately, the orbital period of 16.6 yrexceeds the duration of the mission-limited studies of most space-borneor instrumental-proving observational programs. As with most suchbinaries, the only full-orbit studies are based on photographicmaterials. The last extended study of this system was based upon theplate collections of the McCormick and Sproul Observatories. The workreported here combines data from the Multichannel AstrometricPhotometer, the Hipparcos Intermediate Astrometric Data, the previouslyunmeasured photographic plates of the Allegheny Observatory, publishedobservations of the visual binary, and recently published radialvelocities of the system. Together, these data span more than threeorbits of the low-mass binary system. Limiting our analysis to the mostrecent observations of the binary, and five older observations that arein fair agreement with them, we find masses of 0.2228+/-0.0055 and0.1107+/-0.0028 Msolar for the primary and secondary,respectively, with the largest source of error being the visualseparations of the system. We find a parallax of 244.07+/-0.73 mas, aperiod of 16.595+/-0.0077 yr, and an increased estimate of the semimajoraxis of 1101.2+/-8.2 mas. The latter led to a significant increase inthe computed masses. All other aspects of the orbital elements andastrometry are in excellent agreement with those found in theindependent study of the McCormick and Sproul plates. The importance oflong-term astrometric coverage is pointed out by the fact that theorbital motion of the system only resulted in an acceleration during thecompilation of the Hipparcos Catalogue. No orbital parameters or massestimates can be discerned from these high-precision but short-termdata.
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