The Low-Mass Multiple System GL 831 {Wolf 922}: Definitive Orbit and the Mass- Luminosity Relation

Details The Low-Mass Multiple System GL 831 {Wolf 922}: Definitive Orbit and the Mass- Luminosity Relation The Low-Mass Multiple System GL 831 {Wolf 922}: Definitive Orbit and the Mass- Luminosity Relation

Jul 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000hst..prop.8728f&link_type=abstract

HST Proposal ID #8728

Astronomy and Astrophysics

Astronomy

Hst Proposal Id #8728 Cool Stars

Scientific paper

GL 831 = Wolf 922 {V = 11.98, B-V = 1.67, PI = 0.1258 +/- 0.0023 arcsec} belongs to the select group of about one dozen nearby multiple sytems suitable for calibrating the empirical mass-luminosity relation for masses below 0.2 Msun {Henry et al. 1999}, and has been observed 13 times with FGS3 through Cycle 7. However, a 1.93-yr orbital period, HST scheduling constraints, and a safe mode event conspired to yield repeated coverage of a 180-deg arc about apastron, while leaving unobserved the complementary arc containing periastron {Figure 1}. Consequently, the orbital period is accurate to 0.2 major is known at best to 1.0 these orbital elements yield masses with an accuracy well short of our goal of 5 Cycle 9 provides the first and only opportunity in the next three years to complete the coverage by TRANS mode measures needed to yield a definitive orbit of GL 831 essential for accurate mass determination. We therefore request five orbits as indicated in Figure 1. New POS mode data, combined with those in hand, will yield the mass ratio and a parallax much more accurate than that currently available. Use of FGS1r should also clarify the location and nature of a fainter third component, possibly of 0.1 Msun, detected in two observations with the less capable FGS3.

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