Английская Википедия:DV Piscium
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
DV Piscium is a triple star system[1] in the equatorial constellation of Pisces, abbreviated DV Psc. It is an eclipsing binary variable of the RS Canum Venaticorum class.[2] The pair have a combined apparent visual magnitude of 10.59,[3] which is too faint to be visible with the naked eye. Based on parallax measurements, DV Piscium is located at a distance of 137.5 light years from the Sun.[4] It is drifting closer with a radial velocity of −28 km/s.[5]
In 1994, this target was found to show emission line features in the calcium H and K lines. It was classified as a K-type star with a high proper motion in 1986. Data from the ROSAT satellite showed significant X-ray emission. In 1999, it was shown to be a near-contact eclipsing binary star system by R. M. Robb and associates, with an orbital period of 0.30855 days. The shape of the light curve suggested the presence of one or more star spots on the cooler component.[6] A flare event was observed on November 22, 2008, indicative of a high level of magnetic activity.[7]
Combining photometric results across several years demonstrated that the light curve is highly variable, with star spot activity on both components. These varied over time in quantity, size, and location.[8] This is a detached binary system with the components in near contact at a separation of just two solar radii. As of 2007, the period of the system is decreasing over time at a rate of about Шаблон:Val.[2] The primary component has 68% of the mass of the Sun and 73% of the Sun's radius; the cooler secondary has 47% of the mass and 52% of the radius of the Sun.[1] Both components are slightly evolved main sequence stars. The system has an activity cycle estimated at Шаблон:Val.[9]
Evidence from O–C diagrams suggests there is a third component to this system, orbiting the inner pair with a period of Шаблон:Val on an eccentric orbit. This body has less than 62% of the mass of the Sun.[1]
References
Further reading
- ↑ 1,0 1,1 1,2 Ошибка цитирования Неверный тег
<ref>; для сносокGazeas_Palafouta_2019не указан текст - ↑ 2,0 2,1 Ошибка цитирования Неверный тег
<ref>; для сносокZhang_2007не указан текст - ↑ Ошибка цитирования Неверный тег
<ref>; для сносокSamus_et_al_2017не указан текст - ↑ Ошибка цитирования Неверный тег
<ref>; для сносокGaiaEDR3не указан текст - ↑ Ошибка цитирования Неверный тег
<ref>; для сносокTorres_et_al_2006не указан текст - ↑ Ошибка цитирования Неверный тег
<ref>; для сносокRobb_et_al_1999не указан текст - ↑ Ошибка цитирования Неверный тег
<ref>; для сносокZhang_et_al_2010не указан текст - ↑ Ошибка цитирования Неверный тег
<ref>; для сносокParimucha_et_al_2010не указан текст - ↑ Ошибка цитирования Неверный тег
<ref>; для сносокPalafouta_Gazeas_2020не указан текст
- Английская Википедия
- K-type main-sequence stars
- RS Canum Venaticorum variables
- Eclipsing binaries
- Triple star systems
- Pisces (constellation)
- Objects with variable star designations
- Страницы, где используется шаблон "Навигационная таблица/Телепорт"
- Страницы с телепортом
- Википедия
- Статья из Википедии
- Статья из Английской Википедии
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