參宿四
参考資料

1 2 3 4 5 6  . Centre de Données astronomiques de Strasbourg.   [2007-06-20]. （原始内容存档于2019-05-02）.
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1 2 3 4 5 6 7 8 9 10  Harper, Graham M.; Brown, Alexander; Guinan, Edward F.  (PDF). The Astronomical Journal. April 2008, 135 (4): 1430–40  [2010-07-10]. Bibcode:2008AJ....135.1430H. doi:10.1088/0004-6256/135/4/1430. （原始内容存档 (PDF)于2011-07-15）.
↑  Note:絕對星等的計算依據估計視差測量，會有很大的變化。SIMBAD以参宿四0.42的平均視星等，和197秒差距的距離計算得到的絕對星等是-6.05。参宿四的變光範圍在0.2－1.2，則絕對星等的變化在-6.27－-5.27。
↑  Kaler, James B. (Jim). . Stars website. University of Illinois.   [2009-07-19]. （原始内容存档于2019-09-05）.
↑  See Note #2 for calculations
1 2  Lobel, Alex; Dupree, Andrea K.  (PDF). The Astrophysical Journal,. 2000, December, 545 (1): 454–74  [2010-07-10]. Bibcode:2000ApJ...545..454L. doi:10.1086/317784. （原始内容存档 (PDF)于2011-07-15）.  请检查|date=中的日期值 (帮助)
↑  A luminosity of 140,000 Suns is an imputed figure based on various considerations. Two of the most important variables that influence luminosity calculations are distance（See Enigmatic parallax）and angular separation（See Angular anomalies）. The calculations can be seen in Note #4 with added discussion found at the Luminosity section on the discussion page.
1 2  Kervella, P.; Verhoelst, T.; Ridgway, S. T.; Perrin, G.;  et al. . Astronomy and Astrophysics. September 2009, 504 (1): 115–25  [2010-07-10]. Bibcode:2009A&A...504..115K. doi:10.1051/0004-6361/200912521. （原始内容存档于2012-03-23）.  引文格式1维护：显式使用等标签 (link)
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↑  . IAU Division C Working Group on Star Names (WGSN). International Astronomical Union (IAU).   [28 July 2016]. （原始内容存档于2018-07-07） –University of Rochester.
↑
↑  Stella lucida in umero dextro, quae ad rubedinem vergit. "Bright star in right shoulder, which inclines to ruddiness."
↑  
Brück, H. A. . McCarthy, M.F.; Philip, A.G.D.; Coyne, G.V.  (编). . Spectral Classification of the Future. Vatican City: 7–20. 11–15 July 1978 (1979). Bibcode:1979RA......9....7B.  请检查|publication-date=中的日期值 (帮助)
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Kaler, James B. . New York, NY: Copernicus Books. 2002: 33. ISBN 978-0-387-95436-3.
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Michelson, A.A.; Pease, F.G. . Astrophysical Journal. 1921, 53 (5): 249–259. Bibcode:1921ApJ....53..249M. S2CID 21969744. doi:10.1086/142603. The 0.047 arcsecond measurement was for a uniform disk. In the article Michelson notes that limb darkening would increase the angular diameter by about 17%, hence 0.055 arcseconds.
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Schwarzschild, Martin. . Princeton University Press. 1958. Bibcode:1958ses..book.....S. ISBN 978-0-486-61479-3.  含有內容需登入查看的頁面 (link)
1 2 3  Gilliland, Ronald L.; Dupree, Andrea K.  (PDF). Astrophysical Journal Letters,. May 1996, 463: L29  [2010-08-01]. Bibcode:1996ApJ...463L..29G. doi:10.1086/310043. （原始内容存档 (PDF)于2011-07-15）. 参宿四呈現黃/紅的"影像"或"照片"不是通常所看見的真實的紅巨星影像，而是基於數學方法所生成的影像。其實，這張照片的解析度非常低：整個参宿四的影像在哈伯太空望遠鏡的暗天體照相機上所佔的範圍只有10X10畫素。實際的影像以5倍因素的雙三次曲線內插過度取樣，然後反卷積。
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1 2  Byrd, Deborah. . Earth & Sky. 2019-12-23  [2020-01-04]. （原始内容存档于2022-10-29）.
↑  Overbye, Dennis. . The New York Times. 14 August 2020  [15 August 2020]. （原始内容存档于2022-12-22）. The mysterious dimming of the red supergiant Betelgeuse is the result of a stellar exhalation, astronomers say.
↑   (新闻稿). Hubble Space Telescope. 13 August 2020  [2023-02-03]. （原始内容存档于2023-02-03）.
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1 2  Drake, Nadia. . National Geographic Society. 26 December 2019  [26 December 2019]. （原始内容存档于2021-01-08）. The red giant Betelgeuse is the dimmest seen in years, prompting some speculation that the star is about to explode. Here's what we know.
↑  Kaplan, Sarah. . The Washington Post. 27 December 2019v  [28 December 2019]. （原始内容存档于2022-01-25）.
1 2  Iorio, Kelsie. . ABC News. 27 December 2019  [28 December 2019]. （原始内容存档于2022-12-22）.
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↑   (新闻稿). University of Washington. 6 March 2020  [6 March 2020]. （原始内容存档于2021-02-28） –EurekAlert!.
↑  Levesque, Emily M.; Massey, Philip. . The Astrophysical Journal Letters. 24 February 2020, 891 (2). L37. Bibcode:2020ApJ...891L..37L . S2CID 211296241. arXiv:2002.10463 . doi:10.3847/2041-8213/ab7935 .
↑  Dharmawardena, Thavisha E.; Mairs, Steve; Scicluna, Peter; Bell, Graham; McDonald, Iain; Menten, Karl; Weiss, Axel; Zijlstra, Albert. . The Astrophysical Journal. 2020-06-29, 897 (1): L9. Bibcode:2020ApJ...897L...9D. ISSN 2041-8213. S2CID 219721417. arXiv:2006.09409 . doi:10.3847/2041-8213/ab9ca6.
↑  Sigismondi, Costantino. . The Astronomer's Telegram. 31 March 2020  [1 April 2020]. （原始内容存档于2022-12-22）.
↑  Andrea Dupree; Edward Guinan; William T. Thompson. . Astronomer's Telegram. 28 July 2020  [28 July 2020]. （原始内容存档于2022-12-26）.  已忽略未知参数|collaboration= (帮助)
↑  Sigismondi, Costantino;  et al. . The Astronomer's Telegram. 30 August 2020  [31 August 2020]. （原始内容存档于2022-12-12）.
↑  Montargès M, Cannon E, Lagadec E,  et al. . Nature. 16 June 2021, 594 (7863): 365–368. Bibcode:2021Natur.594..365M. PMID 34135524. S2CID 235460928. arXiv:2201.10551 . doi:10.1038/s41586-021-03546-8.
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↑  Van Loon, J. Th. Kervella, P. , 编. . Betelgeuse Workshop 2012. 2013, 60: 307–316. Bibcode:2013EAS....60..307V. CiteSeerX 10.1.1.759.580 . S2CID 118626509. arXiv:1303.0321 . doi:10.1051/eas/1360036.
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1 2  Robert Nemiroff (MTU) & Jerry Bonnell (USRA). . Today's Astronomy Picture of the Day. 2009-08-05  [2010-11-17]. （原始内容存档于2010-11-21）. Betelgeuse is a candidate to undergo a spectacular supernova explosion almost anytime in the next few thousand years.
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↑  . European Space Agency. 2010-05-04  [2010-07-14]. （原始内容存档于2013-06-30）.
↑  This range of absolute magnitudes assumes an apparent magnitude that varies from 0.2 to 1.2 and a distance of 197 pc.
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↑  Dupree, Andrea K.; Gilliland, Ronald L. . Bulletin of the American Astronomical Society,. December 1995, 27: pp. 1328. Bibcode:1995AAS...187.3201D. Such a major single feature is distinctly different from scattered smaller regions of activity typically found on the Sun although the strong ultraviolet flux enhancement is characteristic of stellar magnetic activity. This inhomogeneity may be caused by a large scale convection cell or result from global pulsations and shock structures that heat the chromosphere."  使用|accessdate=需要含有|url= (帮助) 引文格式1维护：冗余文本 (link)
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1 2 3
1 2  Perrin, G.; Ridgway, S. T.; Coudé du Foresto, V.; Mennesson, B.; Traub, W. A.; Lacasse, M. G. . Astronomy and Astrophysics,. May 2004, 418: 675–85  [2007-08-06]. Bibcode:2004A&A...418..675P. doi:10.1051/0004-6361:20040052. （原始内容存档于2012-04-06）. Assuming a distance of 197±45pc, an angular distance of 43.33±0.04 mas would equate to a radius of 4.3 AU or 920 R☉
↑  Young, John. . University of Cambridge. 2006-11-24  [2007-06-21]. （原始内容存档于2007-06-14）. Images of hotspots on the surface of Betelgeuse taken at visible and infra-red wavelengths using high resolution ground-based interferometers
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↑  Wittkowski, M.  (PDF). European Southern Observatory VLTI. 2007-02-23  [2007-08-29]. （原始内容 (PDF)存档于2011-07-28）.
↑  See Note 1 for detailed list of radii and Note 2 for calculations.
↑  Accurate diameter measurement of Betelgeuse using the VLTI/AMBER instrument.  (PDF). Revista Mexicana de Astronomía y Astrofísica (Serie de Conferencias). November  2009, 37: 179–80  [2010-08-02]. Bibcode:2009RMxAC..37..179H. （原始内容 (PDF)存档于2011-07-15）.
↑  Ron Cowen. . 2009-06-10  [2011-05-12]. （原始内容存档于2011-06-29）. The shrinkage corresponds to the star contracting by a distance equal to that between Venus and the Sun, researchers reported June 9 at an American Astronomical Society meeting and in the June 1 Astrophysical Journal Letters.
↑  Courtland, Rachel. . New Scientist. Reed Business Information Ltd. 2009-06-10  [2010-09-25]. （原始内容存档于2011-08-24）.
↑  Robert Nemiroff (MTU) & Jerry Bonnell (USRA). . Today's Astronomy Picture of the Day. 1999-06-05  [2010-07-10]. （原始内容存档于2010-07-14）.
↑  Robert Nemiroff (MTU) & Jerry Bonnell (USRA). . Today's Astronomy Picture of the Day. 2010-01-06  [2010-07-18]. （原始内容存档于2010-07-14）. Given the ongoing debate and many uncertainties regarding Betelgeuse's actual size, APOD in 2010 reaffirmed the Jovian orbit as a standard metric for the star's radius.