Upsilon4 Eridani
Upsilon4 Eridani is a close binary star system in the constellation Eridanus. It is visible to the naked eye with an apparent visual magnitude of 3.56. Based upon parallax measurements, the pair are located around 54.6 parsecs (178 ly) from the Sun.
| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Eridanus |
| Right ascension | 04h 17m 53.66241s |
| Declination | −33° 47′ 54.0569″ |
| Apparent magnitude (V) | 3.56 |
| Characteristics | |
| Spectral type | B8V + B9.5V |
| U−B color index | −0.36 |
| B−V color index | −0.12 |
| Astrometry | |
| Radial velocity (Rv) | +17.6 km/s |
| Proper motion (μ) | RA: +62.52 mas/yr Dec.: −7.24 mas/yr |
| Parallax (π) | 18.33 ± 0.15 mas |
| Distance | 178 ± 1 ly (54.6 ± 0.4 pc) |
| Absolute magnitude (MV) | −0.20 |
| Orbit | |
| Period (P) | 5.0103250±0.0000008 d |
| Semi-major axis (a) | 1.902±0.006 mas |
| Eccentricity (e) | 0 |
| Inclination (i) | 146.2±0.1° |
| Periastron epoch (T) | 2454407.7214 ± 0.002 JD |
| Semi-amplitude (K1) (primary) | 62.68±0.17 km/s |
| Semi-amplitude (K2) (secondary) | 64.70±0.15 km/s |
| Details | |
| υ4 Eri A | |
| Mass | 3.17±0.07 M☉ |
| Radius | 2.32±0.18 R☉ |
| Luminosity | 100.6±4.3 L☉ |
| Surface gravity (log g) | 4.21±0.07 cgs |
| Temperature | 12,930±440 K |
| Rotational velocity (v sin i) | 19 km/s |
| Age | 146 Myr |
| υ4 Eri B | |
| Mass | 3.07±0.07 M☉ |
| Radius | 2.32±0.18 R☉ |
| Luminosity | 87.4±3.3 L☉ |
| Surface gravity (log g) | 4.21±0.07 cgs |
| Temperature | 12,250 K |
| Other designations | |
| Database references | |
| SIMBAD | data |
This is a double-lined spectroscopic binary star system, which means that the Doppler-shifted spectral lines of both components can be distinguished. The pair have a circular orbit with a period of five days. The system is composed of two B-type main-sequence stars: one has a stellar classification of B8V and the other B9.5V. Both stars show HgMn peculiarities in their spectrum, and their properties are nearly identical. The spin rate of the two stars is synchronized to their orbital period. It is possible that a nearby K-type star is also related.