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HD 66141
Star in the constellation Canis Minor From Wikipedia, the free encyclopedia
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HD 66141 is a single[8] star with a substellar companion in the equatorial constellation of Canis Minor. It has the Bayer designation G Canis Minoris,[6] the Gould designation 50 G. Canis Minoris,[7] and has the HR 3145 identifier from the Bright Star Catalogue.[6] When first catalogued it was in the Puppis constellation and was designated "13 Puppis", but it subsequently migrated to Canis Minor.[9] Bode gave it the Bayer designation of Lambda Canis Minoris.[10]
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Properties
This star has an orange hue and is bright enough to be faintly visible to the naked eye on a dark night, having an apparent visual magnitude of +4.39.[1] It is located at a distance of approximately 260 light years from the Sun based on parallax,[2] and is drifting further away with a radial velocity of +71.6 km/s.[1] The star is considered a member of the thin disk population.[4] It has one known substellar companion, previously believed to be a planet,[11] but now thought to be a likely brown dwarf, with some caveats.[12]
The stellar classification of HD 66141 is K2IIIbFe-0.5:,[3] which indicates an evolved K-type giant star with a mild underabundance of iron. It is an estimated nine billion years old with 0.98 times the mass of the Sun[4] and has expanded to 23.5 times the Sun's radius.[5] Over 2003 to 2012 a starspot was periodically dimming its light.[11] The star is radiating 209 times the luminosity of the Sun from its photosphere at an effective temperature of 4,521 K.[5]
A magnitude 10.32 visual companion was reported by J. Glaisher in 1842. As of 2015, it was located at an angular separation of 224.90 arcseconds along a position angle of 315°.[13]
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Planetary system
From December 2003 to January 2012, the team B.-C. Lee, I. Han, and M.-G. Park observed HD 66141 with "the fiber-fed Bohyunsan Observatory Echelle Spectrograph (BOES) at Bohyunsan Optical Astronomy Observatory (BOAO)".[11]
In 2012, a long-period, wide-orbiting exoplanet was deduced by radial velocity. This was published in November.
However, in 2024, a study using astrometry from the Gaia spacecraft suggest that HD 66141 b is actually a brown dwarf, with a maximum mass estimated at 23.9+7.2
−6.4 MJ, based on a large RUWE in the astrometric solution (which could imply that there is a brown dwarf orbiting HD 66141), but they also note that mechanisms such as calibration errors could also explain the large RUWE. A bayesian analysis combining astrometry and radial velocity also measure an orbital inclination of 17 degrees and an orbital period of 480.7 days (1.316 years).[12]
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References
External links
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