HD 23127
Star in the constellation Reticulum
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HD 23127 is a star in the southern constellation of Reticulum. With an apparent visual magnitude of +8.58[5] it is not visible to the naked eye, but can be viewed with a good pair of binoculars. The star is located at a distance of 307 light years from the Sun based on parallax, and is drifting further away with a radial velocity of ~22 km/s.[5] It has an absolute magnitude of 3.62.[5]
| Observation data Epoch J2000.0 Equinox ICRS | |
|---|---|
| Constellation | Reticulum[1] |
| Right ascension | 03h 39m 23.63799s[2] |
| Declination | −60° 04′ 40.2386″[2] |
| Apparent magnitude (V) | +8.576±0.002[3] |
| Characteristics | |
| Spectral type | G2V[4] |
| B−V color index | 0.701±0.013[3] |
| Astrometry | |
| Radial velocity (Rv) | +21.9±1.7[5] km/s |
| Proper motion (μ) | RA: 73.621±0.042[2] mas/yr Dec.: 142.847±0.045[2] mas/yr |
| Parallax (π) | 10.6258±0.0232 mas[2] |
| Distance | 306.9 ± 0.7 ly (94.1 ± 0.2 pc) |
| Absolute magnitude (MV) | 3.62[5] |
| Details[3] | |
| Mass | 1.208±0.045 M☉ |
| Radius | 1.490±0.104 R☉ |
| Luminosity | 3.01±0.03[6] L☉ |
| Surface gravity (log g) | 4.146±0.054 cgs |
| Temperature | 5,843±52 K |
| Metallicity [Fe/H] | 0.29±0.03 dex |
| Rotation | ~33 days |
| Age | 4.508±0.788 Gyr |
| Other designations | |
| CD−60°762, HD 23127, HIP 17054, SAO 248860, TYC 8867-913-1, GSC 08867-00913[7] | |
| Database references | |
| SIMBAD | data |
This is a G-type main-sequence star with a stellar classification of G2V,[4] which means it is generating energy through core hydrogen fusion. HD 23127 is more massive than the Sun at 1.21 solar masses and has a 49% larger radius. It is metal-rich, having nearly double the abundance of iron in its atmosphere compared to the Sun. This star has an age of 4.5 billion years;[3] about the same as the Sun.
On Friday, February 9, 2007, a 3.32 years period jovian planet was found by using the wobble method by O'Toole and colleagues in Australia.[8] It has minimum mass 53% greater than Jupiter and orbits with a 41% eccentricity. The maximum stable period for a hypothetical inner planet is 322.1 days.[3]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination (°) |
Radius |
|---|---|---|---|---|---|---|
| b | ≥1.527+0.037 −0.038 MJ |
2.370±0.032 | 1,211.17+11.11 −8.91 |
0.406+0.083 −0.09 |
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