03h17m40.0461s, +31° 07′ 37.372″| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Aries |
| Right ascension | 03h17m 40.04683s[1] |
| Declination | +31° 07′ 37.3604″[1] |
| Apparent magnitude (V) | 6.40[2] |
| Characteristics | |
| Spectral type | F8V[2] |
| B−V color index | 0.574[2] |
| Astrometry | |
| Radial velocity (Rv) | 6.47±0.15[1] km/s |
| Proper motion (μ) | RA: −101.950±0.031 mas/yr[1] Dec.: −58.033±0.028 mas/yr[1] |
| Parallax (π) | 38.3758 ± 0.0318 mas[1] |
| Distance | 84.99 ± 0.07 ly (26.06 ± 0.02 pc) |
| Absolute magnitude (MV) | 4.27[3] |
| Details | |
| Mass | 1.13±0.10[4] M☉ |
| Radius | 1.12+0.03 −0.01[5] R☉ |
| Luminosity | 1.576±0.004[5] L☉ |
| Surface gravity (log g) | 4.53±0.22[4] cgs |
| Temperature | 6,100+36 −60[5] K |
| Metallicity [Fe/H] | 0.17±0.10[4] dex |
| Rotational velocity (v sin i) | 5.5[6] km/s |
| Age | 2.98[6] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
| Exoplanet Archive | data |
HD 20367 is a star in the constellationofAries, close to the border with the Perseus constellation. It is a yellow-white hued star that is a challenge to view with the naked eye, having an apparent visual magnitude of 6.40.[2] Based upon parallax measurements, it is located 85 light years from the Sun. It is drifting further away with a radial velocity of +6.5 km/s.[1] Based upon its movement through space, it is a candidate member of the Ursa Major Moving Group of co-moving stars that probably share a common origin.[8]
This object is a late F-type main-sequence star with a stellar classification of F8V.[2] It is about three[6] billion years old and is spinning with a projected rotational velocity of 5.5 km/s.[6] The star is 12%[5] larger and 13%[4] more massive than the Sun. It is radiating 1.58[5] times the luminosity of the Sun from its photosphere at an effective temperature of 6,100 K.[5]
In June 2002, an announcement was made that a Jupiter-mass or larger extrasolar planet had been found orbiting the star,[9] with a period of 1.285 years and an eccentricity of 0.32. The eccentric nature of this planet's orbit meant that it spends part of each circuit around the star outside the habitable zone.[10] However, subsequent observations in 2009 put the existence of this planet in doubt.[11]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b (unconfirmed) | >1.17 MJ | 1.246±0.075 | 469.5±9.3 | 0.320±0.090 | — | — |
|
| |||||||||||||
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| |||||||||||||
| Stars |
| ||||||||||||
| |||||||||||||
| Galaxies |
| ||||||||||||
| |||||||||||||
| |||||||||||||
