Astronomy:HD 202206
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Capricornus[1] |
| Right ascension | 21h 14m 57.76860s[2] |
| Declination | −20° 47′ 21.1615″[2] |
| Apparent magnitude (V) | +8.07±0.01[3] |
| Characteristics | |
| Spectral type | G6V[4] or G2V[5] |
| B−V color index | 0.714±0.012[1] |
| Astrometry | |
| Radial velocity (Rv) | +14.63±0.19[2] km/s |
| Proper motion (μ) | RA: −39.173[2] mas/yr Dec.: −120.068[2] mas/yr |
| Parallax (π) | 21.9392 ± 0.0275[2] mas |
| Distance | 148.7 ± 0.2 ly (45.58 ± 0.06 pc) |
| Absolute magnitude (MV) | +4.80[1] |
| Details[5] | |
| Mass | 1.06+0.07 −0.06 M☉ |
| Radius | 1.04±0.02 R☉ |
| Luminosity | 1.09±0.06 L☉ |
| Surface gravity (log g) | 4.39+0.21 −0.19 cgs |
| Temperature | 5,764+64 −58 K |
| Metallicity [Fe/H] | 0.23+0.12 −0.13 dex |
| Rotational velocity (v sin i) | 2.3±0.5[3] km/s |
| Age | 3.94+1.28 −3.91 Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
| Exoplanet Archive | data |
HD 202206 is a star in the southern constellation of Capricornus. With an apparent visual magnitude of +8.1,[3] it is too faint to be visible to the naked eye. It is located at a distance of 150 light-years from the Sun based on parallax, and is drifting further away with a radial velocity of +14.6 km/s.[2]
This is a G-type main-sequence star with a stellar classification of G6V,[4] indicating it is generating energy through core hydrogen fusion. It is an estimated three[3] billion years old and is spinning with a projected rotational velocity of 2.3 km/s.[3] It is a metal-rich star – what astronomers term the abundance of elements of higher atomic number than helium – which may explain the star's unusually high luminosity for its class.[7] The star has a slightly greater mass and radius compared to the Sun.[3]
Companions
In 2000, analysis of radial velocity measurements of the star revealed the existence of a brown dwarf companion[8] with at least 17 times the mass of Jupiter around the star in an eccentric orbit with a period of around 256 days.[7] Even after the brown dwarf was accounted for, the star still showed a drift in the radial velocity measurements, suggesting another companion in a longer-period orbit. In 2004 after further observations, the parameters of a planetary companion was announced, with a radial velocity semi-amplitude of 42 m/s.[9] The planet is located approximately 3 times further from the star than the brown dwarf and has a mass 3 times that of Jupiter.[5]
Further observation of this system via astrometry with the Hubble Space Telescope revised this picture in 2017, suggesting that the system was viewed nearly face-on and so the companions had true masses much greater than their minimum masses. The system would consist of a pair of co-orbiting stars being viewed nearly face-on, with the pair being orbited in turn by a super-Jupiter designated HD 202206 c. The secondary stellar companion, HD 202206 b, would be a red dwarf star with 8.9% of the mass of the Sun.[3]
However, a subsequent study in 2026 using Gaia DR3 astrometry ruled out the 2017 model of the system and found smaller masses for the companions, closer to the original estimates. The two bodies (brown dwarf and planet) are in a 5:1 mean-motion resonance.[5]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | 21.55+0.80 −0.81 MJ |
0.81+0.01 −0.02 |
256.26±0.03 | 0.426±0.002 | 50.7+25.8 −1.4° |
— |
| c | 3.09±0.14 MJ | 2.39+0.04 −0.05 |
1,299.22+3.21 −2.76 |
0.171+0.021 −0.025 |
50.7+25.8 −1.4° |
— |
References
- ↑ 1.0 1.1 1.2 Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters 38 (5): 331. doi:10.1134/S1063773712050015. Bibcode: 2012AstL...38..331A XHIP record for this object at VizieR.
- ↑ 2.0 2.1 2.2 2.3 2.4 2.5 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940 Gaia DR3 record for this source at VizieR.
- ↑ 3.0 3.1 3.2 3.3 3.4 3.5 3.6 Benedict, G. Fritz; Harrison, Thomas E. (June 2017). "HD 202206: A Circumbinary Brown Dwarf System". The Astronomical Journal 153 (6): 12. doi:10.3847/1538-3881/aa6d59. 258. Bibcode: 2017AJ....153..258B.
- ↑ 4.0 4.1 Houk, N.; Smith-Moore, M. (1988). Michigan Catalogue of Two-dimensional Spectral Types for the HD Stars. 4. Bibcode: 1988mcts.book.....H.
- ↑ 5.0 5.1 5.2 5.3 5.4 Cao, Yingyi; Hoi Lee, Man et al. (June 2026). "Dynamical analysis of the 5:1 mean-motion resonance of the HD 202206 system". Astronomy & Astrophysics. doi:10.1051/0004-6361/202660788. ISSN 0004-6361.
- ↑ "HD 202206". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=HD+202206.
- ↑ 7.0 7.1 Udry, S. et al. (2002). "The CORALIE survey for southern extra-solar planets VIII. The very low-mass companions of HD 141937, HD 162020, HD 168443, HD 202206: Brown dwarfs or "superplanets"?". Astronomy and Astrophysics 390 (1): 267–279. doi:10.1051/0004-6361:20020685. Bibcode: 2002A&A...390..267U.
- ↑ "Exoplanets Galore!" (Press release). Garching, Germany: European Southern Observatory. April 15, 2000. Retrieved December 30, 2012.
- ↑ Correia, A. et al. (2005). "The CORALIE survey for southern extra-solar planets. XIII. A pair of planets around HD202206 or a circumbinary planet?". Astronomy and Astrophysics 440 (2): 751–758. doi:10.1051/0004-6361:20042376. Bibcode: 2005A&A...440..751C.
External links
- HD 202206 on Extrasolar Planets Encyclopaedia
- Extrasolar Planet Interactions by Rory Barnes & Richard Greenberg, Lunar and Planetary Lab, University of Arizona
Coordinates: 
21h 14m 57.79s, −20° 47′ 20.1″
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