HD 4391
| Observation data Epoch J2000 Equinox J2000 |
|
|---|---|
| Constellation | Phoenix |
| Right ascension | 00h 45m 45.5930s[1] |
| Declination | –47° 33′ 07.1438″[1] |
| Apparent magnitude (V) | 5.80[2] |
| Characteristics | |
| Spectral type | G3V[3] |
| B−V color index | +0.64[2] |
| Astrometry | |
| Radial velocity (Rv) | –11.4[4] km/s |
| Proper motion (μ) | RA: 183.99[1] mas/yr Dec.: 78.81[1] mas/yr |
| Parallax (π) | 65.97 ± 0.39[1] mas |
| Distance | 49.4 ± 0.3 ly (15.16 ± 0.09 pc) |
| Details | |
| Mass | 1.22 ± 0.04[5] M☉ |
| Surface gravity (log g) | 4.85[5] cgs |
| Temperature | 5,955[5] K |
| Metallicity [Fe/H] | 0.01[5] dex |
| Rotation | 12 days[6] |
| Rotational velocity (v sin i) | 3.5[3] km/s |
| Age | 1.2[6] Gyr |
| Other designations | |
HD 4391 is a triple star system[8] in the constellation Phoenix that is located at a distance of 48.7 light years from the Sun. The primary has a stellar classification of G3V, which is a G-type main sequence star. The physical properties of this star are similar to the Sun, making it a solar analog. However, it is believed to have 22% greater mass than the Sun and is only 1.2 billion years old.[5] The spectrum for this star displays an abnormally low level of beryllium, which may be the result of some form of mixing process.[6]
No planet has been detected in orbit around this star,[5] nor does it emit a statistically significant excess of infrared radiation that might indicate a debris disk.[9] However, it has two companions that share a common proper motion through space with HD 4391, effectively making it a triple star system. The first, a red dwarf of type M4, lies at an angular separation of 17″ from the primary. The second is a type M5 star at a separation of 49″.[8]
References
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