  | |
| Observation data EpochJ2000 EquinoxJ2000 | |
|---|---|
| Constellation | Cetus[1] |
| Right ascension | 01h 34m 37.77868s[2] |
| Declination | −15° 40′ 34.8987″[2] |
| Apparent magnitude (V) | 5.607[3] |
| Characteristics | |
| Evolutionary stage | main sequence[4] |
| Spectral type | A1V[5] |
| U−Bcolor index | +0.05[6] |
| B−Vcolor index | +0.07[6] |
| Astrometry | |
| Radial velocity (Rv) | +10.30±0.7[7] km/s |
| Proper motion (μ) | RA: +94.351mas/yr[2] Dec.: −3.130mas/yr[2] |
| Parallax (π) | 17.4725±0.547 mas[2] |
| Distance | 187 ± 6 ly (57 ± 2 pc) |
| Absolute magnitude (MV) | +1.75[1] |
| Details | |
| Mass | 1.96±0.04[2] M☉ |
| Radius | 1.711±0.007[2] R☉ |
| Luminosity | 19.12[4] L☉ |
| Surface gravity (log g) | 4.30±0.15[8] cgs |
| Temperature | 8,970±100[8] K |
| Metallicity[Fe/H] | 0.10[4] dex |
| Rotational velocity (v sin i) | 196.9±2.1[8] km/s |
| Age | 40[9] Myr |
| Other designations | |
| BD−16°265,HD 9672,HIP 7345,HR 451,SAO 147886 | |
| Database references | |
| SIMBAD | data |
49 Ceti is a single[10]star in theequatorialconstellation ofCetus. It is visible to the naked eye as a dim, white-hued star with anapparent visual magnitude of 5.607.[3] The star is located 187 light-years (57 parsecs) away from theSolar System, based on itsparallax,[2] and is drifting further away with aradial velocity of +10 km/s.[7] 49 Ceti has been identified as a member of the 40-million-year-oldArgus Association.[9]
This is a youngA-type main-sequence star with astellar classification of A1V.[5] It is about 40 million years old[9] with a high rate of spin, showing aprojected rotational velocity of 196 km/s.[8] The star has 1.96 times themass of the Sun and 1.71 times theradius of the Sun.[2] It is radiating 19 times theSun's luminosity from itsphotosphere at aneffective temperature of 8,790 K.[4][8]
49 Ceti displays a significantinfrared excess, which is a characteristic of adebris disk orbiting the star. Unusually, the disk seems to be gas-rich, with evidence ofcarbon monoxide (CO) gas. This carbon monoxide gas may possibly be fromcomets orbiting the star within the disk, similar to theKuiper Belt in the Solar System.[9]
