Английская Википедия:Gamma Persei

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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 Gamma Persei (Gamma Per, γ Persei, γ Per) is a binary star system in the constellation Perseus. The combined apparent visual magnitude of the pair is +2.9, making it the fourth-brightest member of the constellation. The distance to this system has been measured using the parallax technique, giving an estimate of roughly Шаблон:Convert with a 4% margin of error. About 4° to the north of Gamma Persei is the radiance point for the annual Perseid meteor shower.

Файл:Gamma Persei TESS lightcurve.png

Lightcurve of Gamma Persei's 2019 eclipse recorded by NASA's Transiting Exoplanet Survey Satellite (TESS).

This is a wide eclipsing binary system with an orbital period of 5,329.8 days (14.6 years). This eclipse was first observed in 1990 and lasted for two weeks. During an eclipse, the primary passes in front of the secondary, causing the magnitude of the system to decrease by 0.55. The primary component of this system is a giant star with a stellar classification of G9 III. It has a projected rotational velocity of 50.0 km s⁻¹ and a lengthy estimated rotation period of 14.6 years. The classification of the secondary remains tentative, with assignments of A3 V and A2(III).

Mass estimates for the two stars remain disparate. Using speckle interferometry, McAlister (1982) obtained mass estimates of Шаблон:Solar mass for the primary and Шаблон:Solar mass for the secondary, where Шаблон:Solar mass is the mass of the Sun. He noted that the mass estimate was too high for the given classification of the primary. Martin and Mignard (1998) determined masses for both components based on data from the Hipparcos mission: Шаблон:Solar mass for the primary and Шаблон:Solar mass for the secondary. They admit that the high inclination of the orbit resulted in a large margin of error. Prieto and Lambert (1999) came up with a mass estimate of Шаблон:Solar mass for the primary, while Pizzolato and Maggio (2000) obtained Шаблон:Solar mass. Ling et al. (2001) obtained estimates of Шаблон:Solar mass for the primary and Шаблон:Solar mass for the secondary, while Kaler (2001) obtained 2.5 and 1.9, respectively.

Name and etymology

• This star, together with δ Per, ψ Per, σ Per, α Per and η Per, has been called the Segment of Perseus.
• In Chinese, Шаблон:Lang (Шаблон:Lang), meaning Celestial Boat, refers to an asterism consisting of γ Persei, η Persei, α Persei, ψ Persei, δ Persei, 48 Persei, μ Persei and HD 27084. Consequently, the Chinese name for γ Persei itself is Шаблон:Lang (Шаблон:Lang, Шаблон:Lang-en.)