Английская Википедия:HD 224355

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Файл:Sigma Cassiopeiae.jpg
σ Cassiopeiae with HD 224355 to the right (west)

HD 224355, also known as V1022 Cassiopeiae, HR 9059 and (in early publications) Boss 6148, is an eclipsing binary star in the constellation Cassiopeia. It ranges in apparent magnitude from 5.57 to 5.68, which means it is faintly visible to the naked eye for an observer located well away from city lights.[1] It is one of the few binaries known to be an astrometric, spectroscopic and eclipsing binary, a combination that allows the parameters of the stellar system to be calculated with high accuracy.[2] HD 224355 lies Шаблон:Val west of the 5th-magnitude σ Cassiopeiae.

Файл:V1022CasLightCurve.png
A light curve for HD 224355, plotted from TESS data[3]

HD 224355 was discovered to be a spectroscopic binary by Harry Hemley Plaskett of the DAO, in 1919.[4] Many additional spectra were obtained at the DAO in 1922, and orbital elements of the binary were first published in 1923. The orbit was found to have a significant eccentricity of 0.278.[5] Because the physical separation of spectroscopic binaries is often relatively small, they are good candidates to be eclipsing binaries. For that reason, in 1924 Joel Stebbins included HD 224355 in an early photo-electric photometry study, and observed a "suspect eclipse".[6] That led to the star being listed in the New Catalogue of Suspected Variable Stars as NSV 14773.[7] Hipparcos data confirmed that HD 224355 is an Algol-type eclipsing binary.[8] In 2008 it was given the variable star designation V1022 Cassiopeiae.[9]

From 2014 through 2017, HD 224355 was observed with the CHARA optical interferometer. Those observations allowed the orbit to be directly traced from the changes of the stars' relative positions on the sky. That orbit, when combined with radial velocity information, provided a distance measurement to the star. The value obtained, Шаблон:Val, agrees well with the value of Шаблон:Val measured by the Gaia spacecraft using the completely independent method of stellar parallax.[10]

Both components of the HD 224355 system are slightly more massive than the Sun, F5 or F6 stars 1.9 billion years old and right at the end of their main sequence lives. Each is about 2.5 times the radius of the Sun and 9 or 10 times as luminous, and they have effective temperatures around Шаблон:Val.[11] Шаблон:Clear left

References

Шаблон:Reflist

Шаблон:Stars of Cassiopeia

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  1. ↑ Ошибка цитирования Неверный тег <ref>; для сносок gcvs не указан текст
  2. ↑ Ошибка цитирования Неверный тег <ref>; для сносок Southworth2021 не указан текст
  3. ↑ Ошибка цитирования Неверный тег <ref>; для сносок MAST не указан текст
  4. ↑ Ошибка цитирования Неверный тег <ref>; для сносок Plaskett1920 не указан текст
  5. ↑ Ошибка цитирования Неверный тег <ref>; для сносок Harper1923 не указан текст
  6. ↑ Ошибка цитирования Неверный тег <ref>; для сносок Stebbins1928 не указан текст
  7. ↑ Ошибка цитирования Неверный тег <ref>; для сносок NCSVS не указан текст
  8. ↑ Ошибка цитирования Неверный тег <ref>; для сносок Otero2006 не указан текст
  9. ↑ Ошибка цитирования Неверный тег <ref>; для сносок Kazarovets2008 не указан текст
  10. ↑ Ошибка цитирования Неверный тег <ref>; для сносок Lester2019 не указан текст
  11. ↑ Ошибка цитирования Неверный тег <ref>; для сносок Fekel2022 не указан текст
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