The Masses of the O-type Binary 15 Monocerotis

Details The Masses of the O-type Binary 15 Monocerotis The Masses of the O-type Binary 15 Monocerotis

Jul 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002hst..prop.9346g&link_type=abstract

HST Proposal ID #9346

Astronomy and Astrophysics

Astronomy

Hst Proposal Id #9346 Hot Stars

Scientific paper

The O-type star 15 Mon {HD 47839} was recently discovered to be an astrometric and spectroscopic binary with an orbital period of 25 years; it is the first known O-star system to bridge the observational gap between the period regimes normally probed by these techniques. An analysis of both the radial velocity curve and astrometric orbit yields the masses of the components and distance to the system. Both radial velocity and astrometric measurements are scant at present, but the system is now close to periastron and continued spectroscopic and astrometric monitoring will lead to a definitive orbit and yield important information about the masses of O-type stars. FGS TRANS mode measurements of separation, position angle, and magnitude difference {begun in Cycle 5} are needed to bridge the gap between recent speckle observations and anticipated observations with CHARA Array optical interferometer. In addition, new field astrometry measurements {FGS POS mode} will provide the proper motion, parallax, and the binary motion around the center of mass. The POS data will provide an accurate estimate of the mass ratio and an improved estimate of distance, and taken together with the spectroscopic and astrometric orbital data, we should be able to obtain masses for both components accurate to a few percent.

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