| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Pisces |
| Right ascension | 00h 34m 57.524s[1] |
| Declination | +04° 22′ 53.28″[1] |
| Apparent magnitude (V) | 8.97[2] |
| Characteristics | |
| Evolutionary stage | Main sequence |
| Spectral type | K0 V[3] |
| B−V color index | 0.827±0.021 |
| Variable type | Constant[2] |
| Astrometry | |
| Radial velocity (Rv) | +19.5±0.1[4] km/s |
| Proper motion (μ) | RA: +107.569 mas/yr[1] Dec.: −173.334 mas/yr[1] |
| Parallax (π) | 21.1363 ± 0.0187 mas[1] |
| Distance | 154.3 ± 0.1 ly (47.31 ± 0.04 pc) |
| Absolute magnitude (MV) | 5.67[2] |
| Details[5][6] | |
| Mass | 0.837+0.053 −0.043 M☉ |
| Radius | 0.880+0.012 −0.013 R☉ |
| Luminosity | 0.56[2] L☉ |
| Surface gravity (log g) | 4.47±0.05 cgs |
| Temperature | 5,261±60 K |
| Metallicity [Fe/H] | 0.04±0.05 dex |
| Rotational velocity (v sin i) | 1.7±1.1 km/s |
| Age | 7.8±4.3 Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
HD 3167 is a single,[4] orange-hued star in the zodiac constellation of Pisces that hosts a system with three exoplanets.[8][9] The star is too faint to be seen with the naked eye, having an apparent visual magnitude of 8.97.[2] The distance to HD 3167 can be determined from its annual parallax shift of 21.1363 mas as measured by the Gaia space observatory,[1] yielding a range of 154 light years. It has a relatively high proper motion, traversing the celestial sphere at the rate of 0.204″ per year.[10] Since it was first photographed during the Palomar observatory sky survey in 1953, it had moved over 12.5″ by 2017.[5] The star is moving away from the Earth with an average heliocentric radial velocity of +19.5 km/s.[4]
This is an ordinary K-type main-sequence star with a stellar classification of K0 V[3] and no significant variability.[2] The star has 86% of the mass of the Sun and 86% of the Sun's radius.[5] It is a chromospherically inactive[4] star and is radiating 56%[2] of the Sun's luminosity from its photosphere at an effective temperature of 5,261 K. The spin of the star displays a relatively low projected rotational velocity of around 1.7 km/s. It has a near solar metallicity – a term astronomers use for the proportion of elements other than hydrogen and helium in a stellar atmosphere.[5]
In 2019, a group of astronomers first reported that the orbits of the detected exoplanets hosted by the star are oddly unusual: two planets (HD 3167 c; HD 3167 d) revolve around the star on polar orbits, i.e. orbits that pass over the poles of the star.[11] Later, in October 2021, the third planet (HD 3167 b) was found to orbit around the equator of the star instead, while confirming the other planets' orbital inclinations from the 2019 study.[12][13]
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