| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Capricornus |
| Right ascension | 21h 14m 57.76850s[1] |
| Declination | −20° 47′ 21.1624″[1] |
| Apparent magnitude (V) | +8.07±0.01[2] |
| Characteristics | |
| Spectral type | G6V[3] + M8V[2] |
| B−V color index | 0.714±0.012[4] |
| Astrometry | |
| Radial velocity (Rv) | +14.68±0.23[5] km/s |
| Proper motion (μ) | RA: −39.079[1] mas/yr Dec.: −119.999[1] mas/yr |
| Parallax (π) | 21.7264 ± 0.0651 mas[1] |
| Distance | 150.1 ± 0.4 ly (46.0 ± 0.1 pc) |
| Absolute magnitude (MV) | +4.80[4] |
| Orbit[2] | |
| Period (P) | 256.33 days |
| Semi-major axis (a) | 1.40±0.10 mas |
| Eccentricity (e) | 0.432±0.001 |
| Inclination (i) | 10.9±0.8° |
| Longitude of the node (Ω) | 121±4° |
| Periastron epoch (T) | 2,452,176.14±0.12 JD |
| Argument of periastron (ω) (secondary) | 161.9±0.2° |
| Semi-amplitude (K1) (primary) | 0.567±0.001 km/s |
| Details | |
| A | |
| Mass | 1.07±0.08[2] M☉ |
| Radius | 1.05+0.02 −0.03[1] R☉ |
| Luminosity | 1.084+0.004 −0.005[1] L☉ |
| Surface gravity (log g) | 4.5±0.1[2] cgs |
| Temperature | 5,735+76 −74[1] K |
| Metallicity [Fe/H] | 0.29±0.01[4] dex |
| Rotational velocity (v sin i) | 2.3±0.5[2] km/s |
| Age | 2.9±1.0[2] Gyr |
| B | |
| Mass | 0.089+0.007 −0.006[2] M☉ |
| Other designations | |
| Database references | |
| SIMBAD | data |
HD 202206 is a binary star system in the southern constellation of Capricornus. With an apparent visual magnitude of +8.1,[2] 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 +14.7 km/s.[5]
The primary component is a G-type main-sequence star with a stellar classification of G6V,[3] indicating it is generating energy through core hydrogen fusion. It is an estimated three[2] billion years old and is spinning with a projected rotational velocity of 2.3 km/s.[2] 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.[2]
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