(star system thought to host the first detected exoplanet)
The HD 114762 system hosts an object proposed
as an extra-solar planet candidate which would have been the first
exoplanet discovered, but which has since been classified as a star.
The system is now considered a multiple star system consisting of an
F-type star and two smaller stars, each of the latter two either a
red dwarf or brown dwarf.
The first of the latter two was proposed in 1989, based upon the
radial velocity method, and its existence was confirmed in 1991. Its early
mass determination of 11 Jupiter masses was small enough to
consider it to be a planet, but subsequent observation and
analysis determine it to be far more massive, 147 Jupiter masses.
The defined difference between a red dwarf and a brown dwarf is
whether the object ever has or will experience hydrogen burning, but
this is challenging to determine: their mass ranges overlap and
some spectral types can be either. of the two. A second
small stellar companion (making it a triple star) was discovered
through direct imaging during follow-up observations. This
latest-found companion has a large orbit, making direct imaging of
it effective, while the earlier discovered companion is in a small
orbit, giving it radial velocity cycle short enough to for
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