HD 38529
{{Short description|Binary star system in the constellation Orion}}
{{Starbox begin
| name = HD 38529 A/B
}}
{{Starbox observe 2s
| epoch = J2000.0
| constell = Orion
| component1 = HD 38529 A
| dec1 = {{DEC|+01|10|05.5029}}
| component2 = HD 38529 B
| dec2 = {{DEC|+01|12|47.2640}}
}}
{{Starbox character
| b-v = 0.773 / 0.46{{cn|date=April 2025}}
| u-b =
| variable =
}}
{{Starbox astrometry
| component1 = HD 38529 A
| radial_v = {{val|30.19|0.12}}
| prop_mo_ra = {{val|-77.806}}
| prop_mo_dec = {{val|-141.363}}
| parallax = 23.5714
| p_error = 0.0422
| component2 = HD 38529 B
| radial_v2 = {{val|30.94|0.43}}
| prop_mo_ra2 = {{val|-78.612}}
| prop_mo_dec2 = {{val|-142.084}}
| parallax2 = 23.7139
| p_error2 = 0.0168
| absmag_v2 = +10.23{{cn|date=April 2025}}
}}
{{Starbox detail
| source =
| component1 = HD 38529 A
| temperature = {{val|5619|44}}
| metal_fe = {{val|0.38|0.03}}
| rotation = {{val|37.0|0.4|ul=d}}
| rotational_velocity = {{val|3.20|0.50}}
| component2 = HD 38529 B
| rotation2 =
| age_gyr2 =
}}
{{Starbox catalog
| names = {{odlist | name=RAG 1 | WDS=J05466+0110AB }}
| component1 = HD 38529 A
| names1 = {{odlist | BD=+01°1126 | HIP=27253 | HR=1988 | SAO 113119 | WDS=J05466+0110A }}
| component2 = HD 38529 B
| names2 = {{odlist | 2MASS=J05461937+0112471 | LP=598-99 | WDS=J05466+0110B }}
}}
{{Starbox reference
| Simbad = HD+38529 | sn=A
| Simbad2 = HD+38529B | sn2=B
| NSTED = HD-38529
}}
{{Starbox end}}
HD 38529 (138 G. Orionis) is a binary star system approximately 138 light-years away in the constellation of Orion.
HD 38529 A
HD 38529 A is a yellow subgiant star of spectral type G4IV, though it has also been classified as a main sequence dwarf of type G4V and a borderline giant star of type G8III/IV. It is about 48% 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. Its orbit is probably mildly misaligned with the planetary orbits, by 21−45°.
=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. 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.
In 2003, a massive superjovian HD 38529 c was found orbiting at 3.68 AU with a minimum mass of 12.7 Jupiter masses. 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.
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. The possible third planet was refuted after additional radial velocity measurements were collected. Subsequent astrometric studies have found masses for HD 38529 c ranging from just {{Jupiter mass|10.4}} to {{Jupiter mass|18}}, with the most recent value as of 2025 being {{Jupiter mass|12.9}}.
{{OrbitboxPlanet begin
| name = HD 38529 A
| table_ref = {{Efn|HD 38529 b: Xuan et al. (2020)
HD 38529 c: Feng et al. (2025)
Debrisk disk: Henry et al. (2013)}}
}}
{{OrbitboxPlanet
| exoplanet = b
| mass = {{val|0.8047|0.0139|p=≥}}
| period = {{val|14.30978|0.00033}}
| semimajor = {{val|0.1278|0.0006}}
| eccentricity = {{val|0.259|0.016}}
}}
{{OrbitboxPlanet
| exoplanet = c
| mass = {{val|12.93|0.70|0.49}}
| period = {{val|2127.8|3.3|3.2}}
| semimajor = {{val|3.604|0.043|0.042}}
| eccentricity = {{val|0.3507|0.0057|0.0051}}
| inclination = {{val|104.2|8.9|11}}
}}
{{OrbitboxPlanet disk
| disk = Debris disk
| periapsis = {{val|46|38|27}}
| apoapsis = {{val|208|54}}
| inclination = {{val|71|10|7}}
}}
{{Orbitbox end}}
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. Wide binary stars such as HD 38529 AB have been shown to be vulnerable to disruption by galactic tides and perturbations by passing stars.
See also
Notes
{{notelist}}
References
{{Reflist|refs=
{{cite constellation|HD 38529}}
| url=http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=V%2F135%2Fcatalog
| last=Gould | first=Benjamin Apthorp | date=1879
| title=Uranometria Argentina catalog of bright southern stars
| journal=Resultados del Observatorio Nacional Argentino en Cordoba
| volume=1 | publication-place=Buenos Aires
| bibcode=1879RNAO....1.....G | access-date=2012-05-08
}}
{{Cite Gaia DR3|3219847066672970368}}
{{Cite Gaia DR3|3219851121121855872}}
{{cite simbad | title=WDS J05466+0110AB | access-date=2019-09-07 }}
{{cite simbad | title=HD 38529 | access-date=2019-09-09 }}
{{cite simbad | title=HD 38529 B | access-date=2019-09-09 }}
{{cite journal |last1=Feng |first1=Fabo |last2=Butler |first2=R. Paul |display-authors=etal |date=August 2022 |title=3D Selection of 167 Substellar Companions to Nearby Stars |journal=The Astrophysical Journal Supplement Series |volume=262 |issue=21 |page=21 |doi=10.3847/1538-4365/ac7e57 |arxiv=2208.12720 |bibcode=2022ApJS..262...21F |s2cid=251864022 |doi-access=free }}
{{cite journal |last1=Feng |first1=Fabo |last2=Xiao |first2=Guang-Yao |display-authors=etal |date=April 2025 |title=Lessons learned from the detection of wide companions by radial velocity and astrometry |journal=Monthly Notices of the Royal Astronomical Society |volume= |issue= |pages= |doi= |arxiv=2412.14542}}
}}
External links
- {{cite encyclopedia|url=http://exoplanet.eu/star.php?st=HD+38529|archive-url=https://web.archive.org/web/20070702190411/http://exoplanet.eu/star.php?st=HD+38529|url-status=dead|archive-date=July 2, 2007|encyclopedia=Extrasolar Planets Encyclopaedia|title=Notes for star HD 38529|access-date=14 April 2006}}
- [http://www.lpl.arizona.edu/~rory/research/xsp/dynamics/ Extrasolar Planet Interactions] {{Webarchive|url=https://web.archive.org/web/20160505160348/http://www.lpl.arizona.edu/~rory/research/xsp/dynamics/ |date=2016-05-05 }} by Rory Barnes & Richard Greenberg, Lunar and Planetary Lab, University of Arizona
{{Sky|05|46|34.9120|+|01|10|05.496|138.397}}
{{Stars of Orion}}
Category:M-type main-sequence stars
Category:Orion (constellation)