}}{{Starbox reference
| Simbad = 14+Cet
}}{{Starbox end}}14 Ceti is a single[23] star in the equatorial constellation of Cetus. It is faintly visible to the naked eye under good viewing conditions, having an apparent visual magnitude of 5.84.[3] The distance to 14 Ceti can be estimated from its annual parallax shift of {{Val|17.26|u=arcsecond}},[1] which puts it 189 light years away. It is moving further from the Earth with a heliocentric radial velocity of +11 km/s,[9] having recently come no closer than {{Convert|54.47|pc|ly|0|order=flip|disp=out|abbr=on|lk=off}}.[8]Gray (1989) as well as Houk and Swift (1999) have this star classified as an F-type main-sequence star with a stellar classification of F5 V.[5][6] However, in the 5th revised edition of the Bright Star Catalogue it was classed by Hoffleit and Warren (1991) as a more evolved subgiant star with a class of F5 IV.[30] The absolute magnitude and effective temperature for this star shows that it is entering the Hertzsprung gap, which is occupied by a class of stars that have consumed the hydrogen at their core but have not yet begun hydrogen fusion along a shell surrounding the center.[23]
Evolutionary models for this star give an estimated age of around 2.1[17] billion years with 1.6[3] times the mass of the Sun. It has 2.6[3] times the Sun's radius and is radiating 10.7[3] times the Sun's luminosity from its photosphere at an effective temperature of about 6,583 K.[17] There is a thin convective envelope near its surface.[3] The star has a lower abundance of elements more massive than helium – what astronomers' term the metallicity – compared to the Sun.[17] The projected rotational velocity is a relatively low 5 km/s, but the rotation rate is unknown since the axial tilt hasn't been determined.[3]14 Ceti shows an X-ray emission of {{Val|0.33|e=30|u=erg s−1}}, which is on the high side for an F5 star. Both the corona and chromosphere of this star show indications of a magnetic field, and a surface field was detected in 2009 with a strength of {{Val|−30|ul=G}}. This made it the only known star between classes F0 and F7 to have a Zeeman effect detected. Two possible explanations for this field are that it is a fast rotator with a dynamo-driven field, or that it is a former Ap star.[23] The activity properties of this star make it more likely to be the latter.[4]
References
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