Английская Википедия:II Pegasi

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II Pegasi is a binary star system in the constellation of Pegasus with an apparent magnitude of 7.4 and a distance of 130 light-years. It is a very active RS Canum Venaticorum variable (RS CVn), a close binary system with active starspots.

The primary (II Pegasi A) is a cool subgiant, an orange K-type star. It has begun to evolve off the main sequence and expand.[1] Starspots cover about 40% of its surface. The star produces intense flares observable at all wavelengths.[2]

Its smaller companion (II Pegasi B) is too close to have been observed directly. It is a red dwarf, an M-type main-sequence star. The stars are tidally locked in a very close orbit with a period of 6.7 days and a separation of a few stellar radii.[1]

X-ray flares from II Pegasi A were observed with the Ariel 5 satellite in the 1970s and with later X-ray observatories. In December 2005, a superflare was detected by the Swift Gamma-Ray Burst Mission.[3] It was the largest stellar flare ever seen and was a hundred million times more energetic than the Sun's typical solar flare.[4]

References

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Шаблон:Stars of Pegasus

  1. 1,0 1,1 Ошибка цитирования Неверный тег <ref>; для сносок Berdyugina1997 не указан текст
  2. Ошибка цитирования Неверный тег <ref>; для сносок Covino2000 не указан текст
  3. Ошибка цитирования Неверный тег <ref>; для сносок Osten2007 не указан текст
  4. Шаблон:Cite web