Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
---|---|
Constellation | Cetus |
Right ascension | 02h 44m 07.34928s[1] |
Declination | −13° 51′ 31.3130″[1] |
Apparent magnitude (V) | 4.238[2] |
Characteristics | |
Spectral type | B7 V[3] or B7 IV[4] |
U−B color index | −0.396[2] |
B−V color index | −0.130[2] |
Astrometry | |
Proper motion (μ) | RA: −8.62[1] mas/yr Dec.: −9.07[1] mas/yr |
Parallax (π) | 8.30 ± 0.21 mas[1] |
Distance | 393 ± 10 ly (120 ± 3 pc) |
Absolute magnitude (MV) | −1.16[5] |
Orbit[6] | |
Period (P) | 2,722±14 d |
Eccentricity (e) | 0.0±0.7 |
Periastron epoch (T) | 2444852 ± 29 JD |
Argument of periastron (ω) (secondary) | 0.0° |
Semi-amplitude (K1) (primary) | 4.33±0.25 km/s |
Details[7] | |
π Cet A | |
Mass | 4.4±0.2 M☉ |
Radius | 4.3±0.3 R☉ |
Luminosity | 468 L☉ |
Surface gravity (log g) | 3.8±0.2 cgs |
Temperature | 12,900±400 K |
Metallicity [Fe/H] | 0.28±0.16[8] dex |
Rotational velocity (v sin i) | 20.9±1.2 km/s |
Age | 0.3+0.1 −0.1 Myr |
Other designations | |
Database references | |
SIMBAD | data |
Pi Ceti, Latinized from π Ceti, is the Bayer designation for a star system in the equatorial constellation of Cetus. It is visible to the naked eye with an apparent visual magnitude of 4.238.[2] Observed to have an Earth half yearly parallax shift of 8.30 mas,[1] it is around 393 light years from the Sun.
This is a single-lined spectroscopic binary system with a nearly circular orbit and a period of 7.45 years. The fact that the system has a negligible eccentricity is surprising for such a long period, and may suggest that the secondary is a white dwarf that had its orbit circularized during a mass-transfer event.[6]
The primary, component A, is a normal B-type star[7] that has been given stellar classifications of B7 V[3] and B7 IV.[4] It appears very young – less than half a million years in age – and may still be on a pre-main sequence track. The star shows no magnetic field but it does emit an infrared excess.[7]
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