13 Ceti
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Cetus |
| Right ascension | 00h 35m 14.87968s |
| Declination | −03° 35′ 34.2367″ |
| Apparent magnitude (V) | 5.20 (5.61 + 6.90) |
| Characteristics | |
| Evolutionary stage | Main sequence |
| Spectral type | F6 V + G4 V + K3.5 V |
| B−V color index | 0.567±0.008 |
| Variable type | RS CVn |
| Astrometry | |
| Radial velocity (Rv) | +10.37±0.40 km/s |
| Proper motion (μ) | RA: +408.34 mas/yr Dec.: −35.22 mas/yr |
| Parallax (π) | 47.05±0.67 mas |
| Distance | 69.3 ± 1.0 ly (21.3 ± 0.3 pc) |
| Absolute magnitude (MV) | 3.56 |
| Orbit | |
| Primary | A |
| Companion | B |
| Period (P) | 2,516.6163±2.7808 d |
| Eccentricity (e) | 0.77300 |
| Periastron epoch (T) | 56,935.2034 MJD |
| Argument of periastron (ω) (secondary) | 283.8°° |
| Orbit | |
| Primary | Aa |
| Companion | Ab |
| Period (P) | 2.081891±0.000005 d |
| Semi-major axis (a) | ≥1.260±0.010 Mm |
| Eccentricity (e) | 0.0 (fixed) |
| Periastron epoch (T) | 2,443,400.4573±0.0032 HJD |
| Argument of periastron (ω) (secondary) | 0.0° |
| Semi-amplitude (K1) (primary) | 43.98±0.39 km/s |
| Details | |
| Aa | |
| Mass | 1.18±0.09 M☉ |
| Luminosity | 2.63 L☉ |
| Temperature | 6,457 K |
| Age | 3.8+1.8 −0.3 Gyr |
| B | |
| Mass | 0.90±0.09 M☉ |
| Luminosity | 0.83 L☉ |
| Temperature | 5,754 K |
| Age | 2.5 Gyr |
| Other designations | |
| HO 212, 13 Cet, BU Cet, NSV 212, BD−04°62, GC 696, GJ 23, HD 3196, HIP 2762, HR 142, SAO 128839, WDS 00352-0336 | |
| Database references | |
| SIMBAD | data |
13 Ceti is a triple star system in the equatorial constellation of Cetus. It is dimly visible to the naked eye with a combined apparent visual magnitude of 5.20. The system is located at a distance of approximately 69 light years from the Sun based on stellar parallax, and is drifting further away with a radial velocity of +10.4 km/s. It shares a common motion with the Hyades moving group, although it is too old to be a member.
This star was identified as a visual binary system by G. W. Hough in 1844 and given the identifier HO 212. The pair have an orbital period of 6.9 years and an eccentricity of 0.77. The brighter member, designated component A, is an F-type main-sequence star with a stellar classification of F6 V and a visual magnitude of 5.61. It appears to have an active chromosphere and is classified as an RS Canum Venaticorum variable with a variable star designation of BU Cet. The star was detected as a source of soft X-ray emission by EXOSAT. It has 18% more mass than the Sun and is estimated to be about four billion years old.
In 1907, E. B. Frost discovered the primary is a spectroscopic binary, making this a triple star system. This is a double-lined spectroscopic binary with a period of 2.1 days and a circularized orbit. The companion signature was confirmed using the separated fringe packet technique with the CHARA array. It is most likely a K-type main-sequence star with a class of K3.5 V and 70% of the mass of the Sun.
The secondary member of the visual binary, designated component B, is a G-type main-sequence star with a class of G4 V. It has 90% of the Sun's mass and a visual magnitude of 6.90. A distant visual companion to this system was detected by S. W. Burnham in 1877. Designated component C, this star is a background object of magnitude 12.50. As of 1999, it was located at an angular separation of 24.0″ from the primary along a position angle of 322°.