HD 38529
Coordinates: 
05h 46m 34.9120s, +01° 10′ 05.496″
05h 46m 34.9120s, +01° 10′ 05.496″| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Orion |
| HD 38529 A | |
| Right ascension | 05h 46m 34.91314s[1] |
| Declination | +01° 10′ 05.5029″[1] |
| Apparent magnitude (V) | +5.94 |
| HD 38529 B | |
| Right ascension | 05h 46m 19.37663s[2] |
| Declination | +01° 12′ 47.2640″[2] |
| Apparent magnitude (V) | +13.35 |
| Characteristics | |
| Spectral type | G4IV / M3.0V |
| U−B color index | ? / ? |
| B−V color index | 0.773 / 0.46 |
| Variable type | none / ? |
| Absolute magnitude (MV) | +10.23 |
| Details Gyr | |
| Database references | |
| SIMBAD | data |
HD 38529 (138 G. Orionis) is a binary star approximately 138 light-years away in the constellation of Orion.
HD 38529 A
HD 38529 A is a yellow subgiant star, which has also been classified as a main sequence dwarf of spectral type G4V. It is about 40% more massive than the Sun. 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.[8] Its orbit is probably mildly misaligned with the planetary orbits, by 21−45°.[9]
Planetary system
In 2002, the planet
true mass 37 times that of Jupiter, turning this planet into a brown dwarf.[12] 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.[13] The possible third planet was refuted after additional radial velocity measurements were collected.[3] A 2022 study estimated an even lower mass of 10.4 Jupiter masses for HD 38529 c. The authors state that their mass estimate is consistent with previous estimates, but with higher precision.[14]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | ≥0.8047±0.0139 MJ | 0.1278±0.0006 | 14.30978±0.00033 | 0.259±0.016 | — | — |
| c | 10.380+1.025 −0.884 MJ |
3.226+0.131 −0.144 |
2127.6+1.5 −1.6 |
0.357±0.005 | 104.559+6.393 −8.722° |
— |
| Debris disk | >86 AU | — | — | |||
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.[15] Wide binary stars such as HD 38529 AB have been shown to be vulnerable to disruption by galactic tides and perturbations by passing stars.[16]
See also
- List of extrasolar planets
- HD 168443
References
- ^ S2CID 244398875. Gaia DR3 record for this source at VizieR.
- ^ S2CID 244398875. Gaia DR3 record for this source at VizieR.
- ^ .
- S2CID 222378164
- ^ "WDS J05466+0110AB". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-09-07.
- ^ "HD 38529". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-09-09.
- ^ "HD 38529 B". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-09-09.
- doi:10.1086/529027.
- S2CID 222177269
- doi:10.1086/320224.
- doi:10.1086/367889.
- hdl:1887/7483.
- .
- ^ S2CID 251864022.
- doi:10.1086/504823.
- hdl:11336/41265.
External links
- "Notes for star HD 38529". Extrasolar Planets Encyclopaedia. Archived from the original on July 2, 2007. Retrieved 14 April 2006.
- Extrasolar Planet Interactions by Rory Barnes & Richard Greenberg, Lunar and Planetary Lab, University of Arizona
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