HD 219077
| Observation data Epoch J2000.0 Equinox J2000.0 |
|
|---|---|
| Constellation | Tucana |
| Right ascension | 23h 14m 06.585s[1] |
| Declination | –62° 42′ 00.02″[1] |
| Apparent magnitude (V) | +6.12 |
| Characteristics | |
| Spectral type | G8V |
| Astrometry | |
| Proper motion (μ) | RA: 476.56 ± 0.31[1] mas/yr Dec.: –425.40 ± 0.29[1] mas/yr |
| Parallax (π) | 34.07 ± 0.37[1] mas |
| Distance | 96 ± 1 ly (29.4 ± 0.3 pc) |
| Details | |
| Mass | 1.05 ± 0.02 M☉ |
| Radius | 1.91 ± 0.03 R☉ |
| Luminosity | 2.66 L☉ |
| Surface gravity (log g) | 4.00 ± 0.03 cgs |
| Temperature | 5362 ± 18 K |
| Metallicity [Fe/H] | –0.13 ± 0.01 dex |
| Age | 8.9 ± 0.3 Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
| Exoplanet Archive | data |
| Extrasolar Planets Encyclopaedia |
data |
HD 219077 is a G-class yellow 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 219077 b is among the "three most eccentric planets with a period larger than 5 years" - along with HD 98649 b and HD 166724 b, also found in CORALIE. The reason for this eccentricity is unknown. They submit HD 219077 b as a "candidate for direct imaging", once it gets out to "11.0 AU at apoastron", and 375 milliarcseconds of separation relative to Earth.[2]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | >10.39 ± 0.09 MJ | 6.22 ± 0.09 | 5501+130 −119 |
0.770 ± 0.003 | — | — |
References
External links
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