Английская Википедия:14 Ceti
Шаблон:Short description Шаблон:Starbox begin Шаблон:Starbox observe Шаблон:Starbox character Шаблон:Starbox astrometry Шаблон:Starbox detail Шаблон:Starbox catalog Шаблон:Starbox reference Шаблон:Starbox end
14 Ceti is a single[1] 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.[2] The distance to 14 Ceti can be estimated from its annual parallax shift of Шаблон:Val,[3] which puts it 187 light years away. It is moving further from the Earth with a heliocentric radial velocity of +11 km/s,[4] having recently come no closer than Шаблон:Convert.[5]
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.[6][7] 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.[8] 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.[1]
Evolutionary models for this star give an estimated age of around 2.1[9] billion years with 1.6[2] times the mass of the Sun. It has 2.6[2] times the Sun's radius and is radiating 10.7[2] times the Sun's luminosity from its photosphere at an effective temperature of about 6,583 K.[9] There is a thin convective envelope near its surface.[2] The star has a lower abundance of elements more massive than helium – what astronomers' term the metallicity – compared to the Sun.[9] 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.[2]
14 Ceti shows an X-ray emission of Шаблон:Val, 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 Шаблон:Val. 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.[1] The activity properties of this star make it more likely to be the latter.[10]
References
- ↑ 1,0 1,1 1,2 Ошибка цитирования Неверный тег
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<ref>; для сносокGray1989не указан текст - ↑ Ошибка цитирования Неверный тег
<ref>; для сносокHouk1999не указан текст - ↑ Ошибка цитирования Неверный тег
<ref>; для сносокHoffleit1995не указан текст - ↑ 9,0 9,1 9,2 Ошибка цитирования Неверный тег
<ref>; для сносокBensby2014не указан текст - ↑ Ошибка цитирования Неверный тег
<ref>; для сносокAurière2014не указан текст
- Английская Википедия
- F-type main-sequence stars
- F-type subgiants
- Hertzsprung gap
- Cetus
- Bright Star Catalogue objects
- Durchmusterung objects
- Henry Draper Catalogue objects
- Hipparcos objects
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- Википедия
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