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Список крупнейших звезд

Ниже приведены списки крупнейших известных на данный момент звезд, упорядоченные по радиусу и разделенные на категории по галактикам. Единицей измерения является радиус Солнца (приблизительно 695 700  км ; 432 300  миль ). [1]

Солнце , орбиты Земли , Юпитера и Нептуна в сравнении с четырьмя звездами ( Звезда Пистолет , Ро Кассиопеи , Бетельгейзе и VY Большого Пса )

Обзор

Хотя красные сверхгиганты часто считаются самыми большими звездами, было обнаружено, что некоторые другие типы звезд временно значительно увеличивают свой радиус, например, во время извержений LBV или светящихся красных новых . Светящиеся красные новые, по-видимому, расширяются чрезвычайно быстро, достигая тысяч или десятков тысяч солнечных радиусов всего за несколько месяцев, что значительно больше, чем у самых больших красных сверхгигантов. [2]

Некоторые исследования используют модели, которые предсказывают, что высокоаккрецирующие сверхмассивные звезды (SMS) Популяции III или Популяции I в очень ранней Вселенной могли бы развиться в «красных сверхгигантских протозвезд». Считается, что эти протозвезды имеют темпы аккреции, превышающие темпы сжатия, что приводит к более низким температурам, но с радиусами, достигающими многих десятков тысяч R ☉ , что сопоставимо с некоторыми из крупнейших известных черных дыр . [3] [4] [5]

Угловые диаметры

Угловые диаметры звезд можно измерить напрямую с помощью звездной интерферометрии . Другие методы могут использовать лунные покрытия или затменные двойные , которые можно использовать для проверки косвенных методов нахождения звездных радиусов. Только несколько сверхгигантов могут быть закрыты Луной, включая Антарес и 119 Тельца . Примерами затменных двойных являются Эпсилон Возничего (Алмааз), VV Цефея и V766 Центавра (HR 5171). Измерения углового диаметра могут быть непоследовательными, поскольку граница очень разреженной атмосферы ( непрозрачность ) отличается в зависимости от длины волны света, в которой наблюдается звезда . [ необходима цитата ]

Неопределенности остаются с составом и порядком списков, особенно при выводе различных параметров, используемых в расчетах, таких как звездная светимость и эффективная температура . Часто звездные радиусы могут быть выражены только как среднее значение или находиться в большом диапазоне значений. Значения звездных радиусов значительно различаются в разных источниках и для разных методов наблюдения. [ необходима цитата ]

Все размеры, указанные в этих списках, имеют неточности и могут быть оспорены. Списки все еще находятся в стадии разработки, и параметры могут измениться.

Предостережения

Существуют различные проблемы с определением точных радиусов крупнейших звезд, которые во многих случаях показывают значительные ошибки. Следующие списки, как правило, основаны на различных соображениях или предположениях; они включают:

Списки

В следующих списках показаны самые крупные известные звезды в зависимости от родительской галактики.

Млечный Путь

Магеллановы Облака

Галактики Андромеды (M31) и Треугольника (M33)

Другие галактики (внутри Местной группы)

За пределами Местной группы (внутри сверхскопления Девы)

За пределами сверхскопления Девы

Обратите внимание, что в этот список не включены кандидаты на роль темных звезд JWST с предполагаемыми радиусами до 61 астрономической единицы (13 000  R ☉ ) [142] или квазизвезды с теоретическими моделями, предполагающими, что они могут достигать радиусов до 40 700 солнечных радиусов (189 а.е.) [143] .

Transient events

During some transient events, such as red novae or LBV eruptions the star's radius can increase by a significant amount.

SN Progenitors

Largest stars by apparent size

The following list include the largest stars by their apparent size (angular diameter) as seen from Earth. The unit of measurement is the milliarcsecond (mas), equivalent to 10×10−3 arcseconds. Stars with angular diameters larger than 13 milliarcseconds are included.

See also

Notes

  1. ^ a b c d e f Methods for calculating the radius:
  2. ^ a b c d e f At the J2000 epoch
  3. ^ [9][10][11][12][13]
  4. ^ Using an angular diameter of 7.8±0.64 milliarcseconds[27] and a distance of 1610+130
    −110     parsecs.    [28]
  5. ^ Luminosities are calculated using the apparent bolometric magnitude and distances in the following equation:
    100.4 • (4.74−(mbol+5−5 • log(dist)))
  6. ^ Using an angular diameter of 14.11±0.6 milliarcseconds and a distance of 940+140
    −40     parsecs.
  7. ^ Calculated using a distance of 432 parsecs and an angular diameter of 2.31 milliarcseconds.
  8. ^ Legend:
    UD=Uniform disk diameter
    LD=Limb-darkened diameter
    Ross=Rosseland diameter
    Est = Estimated using distance and physical radius

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