HD 166724
| Observation data Epoch J2000.0 Equinox J2000.0 |
|
|---|---|
| Constellation | Corona Australis |
| Right ascension | 18h 13m 59.676s[1] |
| Declination | –42° 34′ 31.35″[1] |
| Apparent magnitude (V) | +9.33 |
| Characteristics | |
| Spectral type | K0IV |
| Astrometry | |
| Proper motion (μ) | RA: 36.60 ± 1.59[1] mas/yr Dec.: –78.62 ± 0.99[1] mas/yr |
| Parallax (π) | 23.63 ± 1.21[1] mas |
| Distance | 138 ± 7 ly (42 ± 2 pc) |
| Details | |
| Mass | 0.81 ± 0.02 M☉ |
| Radius | 0.81 ± 0.02 R☉ |
| Luminosity | 0.31 L☉ |
| Surface gravity (log g) | 4.41 ± 0.04 cgs |
| Temperature | 5362 ± 29 K |
| Metallicity [Fe/H] | –0.09 ± 0.03 dex |
| Age | 4.0 ± 3.8 Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
| Exoplanet Archive | data |
| Extrasolar Planets Encyclopaedia |
data |
HD 166724 is a K-class dwarf star.
Planetary system
From 1998 to 2012, the star was under observance from "the CORALIE echelle spectrograph at La Silla Observatory".
In 2012, a long-period, wide-orbiting planet was deduced by radial velocity. This was published in November.
The discoverers noted that HD 166724 b is among "the three most eccentric planets with a period larger than 5 years" alongside HD 98649 b and HD 219077 b; but unlike them, too dim as a candidate for direct imaging with current technology. The reason for this eccentricity is unknown.[2]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | >3.53 ± 0.11 MJ | 5.42 ± 0.43 | 5144+705 −467 |
0.734 ± 0.020 | — | — |
References
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