Английская Википедия:4 Canum Venaticorum
Шаблон:Short description Шаблон:Starbox begin Шаблон:Starbox image Шаблон:Starbox observe Шаблон:Starbox character Шаблон:Starbox astrometry Шаблон:Starbox orbit Шаблон:Starbox detail Шаблон:Starbox catalog Шаблон:Starbox reference Шаблон:Starbox end
4 Canum Venaticorum is a binary star system in the northern constellation of Canes Venatici, located around 425 light years away.[1] It has the variable star designation AI Canum Venaticorum; 4 Canum Venaticorum is its Flamsteed designation. Its brightness varies from magnitude +5.89 to +6.15 with a period of 2.8 hours,[2] which places it around the lower limit of visibility to the naked eye. This was found to be a binary by Schmid et al. in 2014, based on periodic, non-sinusoidal changes in its radial velocity. It is a single-lined spectroscopic binary with an orbital period of 124.4 days and an eccentricity of 0.31.[3]
The primary component is an evolved F-type star with a stellar classification of F3 IV[4] or F0 III,[5] matching a subgiant or giant star, respectively. It is a variable of the Delta Scuti class, displaying both radial and non-radial pulsations.[6] The variable nature of this star was discovered by D. H. P. Jones and C. Margaret Haslam in 1966 at the suggestion of Olin J. Eggen,[7] and it has become one of the best studied stars in its class. The radial pulsations have shown little if any variations between 1974 and 2012. However, the non-radial pulsations vary continuously in frequency over periods spanning decades.[6] It is spinning rapidly with a rotation of at least one third of its critical velocity.[3]
References
Шаблон:Stars of Canes Venatici
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- Английская Википедия
- F-type subgiants
- F-type giants
- Delta Scuti variables
- Spectroscopic binaries
- Canes Venatici
- Durchmusterung objects
- Flamsteed objects
- Henry Draper Catalogue objects
- Hipparcos objects
- Bright Star Catalogue objects
- Objects with variable star designations
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