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HD 38529
Binary star system in the constellation Orion From Wikipedia, the free encyclopedia
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HD 38529 (138 G. Orionis)[13] is a binary star system approximately 138 light-years away in the constellation of Orion.
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HD 38529 A
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HD 38529 A is a yellow subgiant star of spectral type G4IV,[14] though it has also been classified as a main sequence dwarf of type G4V[5] and a borderline giant star of type G8III/IV.[15] It is about 48% more massive than the Sun.[6]
Two substellar companions are known in orbit around this star, including one with a mass near the deuterium fusion limit that is often used as the dividing line between giant planets and brown dwarfs. There is a debris disk located at least 86 astronomical units from the star.[16] Its orbit is probably mildly misaligned with the planetary orbits, by 21−45°.[17]
Planetary system
In 2001, the planet HD 38529 b was discovered orbiting the star HD 38529 A by Debra Fischer and collaborators who detected it using the Doppler spectroscopy technique.[14] It has a mass at least 78% that of Jupiter and orbits very close to the star, just beyond the distance limit for hot Jupiters. It does not transit the star.[7]
In 2003, a massive superjovian HD 38529 c was found orbiting at 3.68 AU with a minimum mass of 12.7 Jupiter masses.[3] Astrometric measurements from the Hipparcos satellite gave a best fit inclination of 160° and a true mass 37 times that of Jupiter, turning this planet into a brown dwarf.[18]
Further study of the system using Hubble Space Telescope astrometry revised the mass of HD 38529 c downwards to 17.7 Jupiter masses and suggested the presence of an additional planet, orbiting in the gap between HD 38529 b and c.[19] The possible third planet was refuted after additional radial velocity measurements were collected.[7] Subsequent astrometric studies have found masses for HD 38529 c ranging from just 10.4 MJ[20] to 18 MJ,[17] with the most recent value as of 2025 being 12.9 MJ.[21]
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HD 38529 B
HD 38529 B is a common proper motion stellar companion to HD 38529 A at a projected distance of about ~12000 astronomical units. The star is a red dwarf of spectral type M3.0V.[5] Wide binary stars such as HD 38529 AB have been shown to be vulnerable to disruption by galactic tides and perturbations by passing stars.[22]
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