Dynamical Masses for the Stars in the Pre -Main- Sequence Spectroscopic Binary 045251+3016

Details Dynamical Masses for the Stars in the Pre -Main- Sequence Spectroscopic Binary 045251+3016 Dynamical Masses for the Stars in the Pre -Main- Sequence Spectroscopic Binary 045251+3016

Dec 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997hst..prop.7485m&link_type=abstract

HST Proposal ID #7485

Astronomy and Astrophysics

Astronomy

Hst Proposal Id #7485 Young Stars And Circumstellar Material

Scientific paper

We propose to use the Fine Guidance Sensors to measure dynamical masses for the two stars in the pre-main-sequence binary 045251+3016 =GSC2387 535. We have already completed an excellent single-lined spectroscopic orbit, which provides all of the essential orbital elements except inclination angle and mass ratio. We will use the FGS to derive both the apparent relative orbit of the binary {giving the inclination angle} and the absolute orbits of both components {giving the mass ratio}. The predicted separation during Cycles 6-7 is > 20 mas, so this experiment is well suited to the FGS. This project was initially allocated 6 orbits in each of Cycles 5, 6 and 7. We have reduced the TRANS scans of our Cycle 5 observations, which successfully resolved the binary. Continued observations in Cycles 6 and 7 are required to obtain the astrometric orbital elements necessary to derive the stellar masses. These observations will provide the first dynamical mass measurements for stars on their Hayashi tracks. In particular, the completed spectroscopic orbital solution makes this a unique opportunity for such measurements independent of any assumptions about the stars or their distance. These measurements are fundamental tests of pre-main -sequence stellar evolution theory.

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