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**人馬座V4332**
	; 人馬座V4332結合可見光通道的光變曲線。主要的情節改編自泰倫達（Tylenda）等人的數據（2015），顯示了長期變化；插圖改編自馬提尼（Martini）等人的數據（1999），顯示了噴發爆發前幾周的變化。
觀測資料; 曆元 J2000.0
星座	人馬座
星官
赤經	18h 50m 36.696s
赤緯	–21° 23′ 28.93″
視星等（V）	8.5
特性
光谱分类	K8/M0e
天体测定
自行 (μ)	赤经：−2.722 mas/yr ; 赤纬：−5.555 mas/yr
视差 (π)	0.0017 ± 0.2798 mas
距离	(3.71±3.3)×103 ly
其他命名
	V4332 Sgr、Nova Sgr 1994
參考資料庫
SIMBAD	资料

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人馬座V4332是在星座人馬座中類似新星事件。它於1994年2月24日由在日本愛知岡崎的業餘天文學家山本實（Minoru Yamamoto）發現，視星等為8.9等，隨後由廣澤（K.Hirosawa）證實^[7]。最初命名為新星人馬座1994#1，並依據變星命名法命名為人馬座^[2]。3月4日拍攝的事件的光譜缺乏經典新星的特徵，唯一的發射線是氫光譜的巴耳末系^[8]。隨後的光譜顯示光度在五天內迅速下降，光譜類型發生變化^[2]。到2003年，該天體的亮度比峰值時的星等低約1,500倍，並顯示出M型恆星的光譜^[9]。

類似新星的事件麒麟座V838和這次爆發形成了一類不同尋常的噴發恒星。2003年，N.Soker和R.Tylenda提出了一個吸積的場景作為解釋。他們指出，在一個封閉的雙星軌道上合併兩顆主序星可以解釋觀測到的性質^[10]，這一過程現在被稱為亮紅新星。在這種情況下，人馬座V4332的亮度和半徑的下降是合併後的恆星外殼經歷引力收縮的結果^[9]。

來自該物體的紅外過量表明它有一個星周盤。該特徵的紅外光譜顯示出水冰的吸收帶和一氧化碳發射帶^[9]。到2010年，恆星成分已經被邊緣觀察到的塵土飛揚的圓盤所掩蓋^[1]。這種灰塵的重要成分包括氧化鋁，與含量不斷增加的氧化鎂和氧化鐵^[11]。

參考資料

^ ^1.0 ^1.1 Tylenda, R.; et al, VLT/UVES spectroscopy of V4332 Sagittarii in 2005: The best view on a decade-old stellar-merger remnant, Astronomy & Astrophysics, June 2015, 578: 14, Bibcode:2015A&A...578A..75T, S2CID 54789582, arXiv:1412.7822 , doi:10.1051/0004-6361/201425592, A75.
^ ^2.0 ^2.1 ^2.2 ^2.3 Martini, Paul; et al, Nova Sagittarii 1994 1 (V4332 Sagittarii): The Discovery and Evolution of an Unusual Luminous Red Variable Star, The Astronomical Journal, August 1999, 118 (2): 1034–1042, Bibcode:1999AJ....118.1034M, S2CID 13862209, arXiv:astro-ph/9905016 , doi:10.1086/300951.
^ ^3.0 ^3.1 ^3.2 Brown, A. G. A.; et al. Gaia Early Data Release 3: Summary of the contents and survey properties. Astronomy & Astrophysics. 2021, 649: A1. Bibcode:2021A&A...649A...1G. S2CID 227254300. arXiv:2012.01533 . doi:10.1051/0004-6361/202039657 . 已忽略未知参数|collaboration= (帮助) (勘误: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
^ Kimeswenger, S., V4332 Sgr in 'Quiescence', Astronomische Nachrichten, January 2006, 327 (1): 44–52, Bibcode:2006AN....327...44K, S2CID 118936262, arXiv:astro-ph/0509844 , doi:10.1002/asna.200510482.
^ Özdönmez, Aykut; et al, The distances of the Galactic novae, Monthly Notices of the Royal Astronomical Society, September 2016, 461 (2): 1177–1201, Bibcode:2016MNRAS.461.1177O, arXiv:1606.01907 , doi:10.1093/mnras/stw1362.
^ V4332 Sgr. SIMBAD. 斯特拉斯堡天文資料中心.
^ Hayashi, S. S.; et al, Marsden, B. G. , 编, Nova Sagittarii 1994, IAU Circular, February 1994, 5942 (1): 1, Bibcode:1994IAUC.5942....1H.
^ Wagner, R. M.; et al, Marsden, B. G. , 编, Nova Sagittarii 1994, IAU Circular, March 1994, 5944 (1): 1, Bibcode:1994IAUC.5944....1W.
^ ^9.0 ^9.1 ^9.2 Tylenda, R.; et al, V4332 Sagittarii revisited, Astronomy and Astrophysics, August 2005, 439 (2): 651–661, Bibcode:2005A&A...439..651T, S2CID 119410176, arXiv:astro-ph/0412205 , doi:10.1051/0004-6361:20041581.
^ Soker, Noam; Tylenda, Romuald, Main-Sequence Stellar Eruption Model for V838 Monocerotis, The Astrophysical Journal, January 2003, 582 (2): L105–L108, Bibcode:2003ApJ...582L.105S, S2CID 18351411, arXiv:astro-ph/0210463 , doi:10.1086/367759.
^ Banerjee, Dipankar. P. K.; et al, Evolution of the Dust in V4332 Sagittarii, The Astrophysical Journal, December 2015, 814 (2): 9, Bibcode:2015ApJ...814..109B, S2CID 119299700, arXiv:1510.05074 , doi:10.1088/0004-637X/814/2/109, 109.

進階讀物

Goranskij, V. P.; et al, Rapid re-brightening of the red nova V4332 Sgr remnant, The Astronomer's Telegram, June 2018, 11733 (11733): 1, Bibcode:2018ATel11733....1G.
Kamiński, T.; Tylenda, R., Optical spectropolarimetry of V4332 Sagittarii, Astronomy & Astrophysics, October 2013, 558: 7, Bibcode:2013A&A...558A..82K, S2CID 119273390, arXiv:1309.0635 , doi:10.1051/0004-6361/201321852, A82.
Kamiński, T.; Tylenda, R., Strong linear polarization of V4332 Sagittarii: a dusty disc geometry, Astronomy & Astrophysics, March 2011, 527: 3, Bibcode:2011A&A...527A..75K, S2CID 55219492, arXiv:1101.1267 , doi:10.1051/0004-6361/201015950, A75.
Kamiński, T.; et al, V4332 Sagittarii: a circumstellar disc obscuring the main object, Astronomy and Astrophysics, November 2010, 522: 12, Bibcode:2010A&A...522A..75K, S2CID 55759155, arXiv:1007.0131 , doi:10.1051/0004-6361/201014406, A75.
Banerjee, D. P. K.; et al, Spitzer Observations of V4332 Sagittarii: Detection of Alumina Dust, The Astrophysical Journal, September 2007, 666 (1): L25–L28, Bibcode:2007ApJ...666L..25B, S2CID 7492121, arXiv:0707.3119 , doi:10.1086/521528.
Goranskij, V.; et al, Unexpected change in the spectrum of V4332 Sgr, The Astronomer's Telegram, August 2006, 876 (876): 1, Bibcode:2006ATel..876....1G.
Lynch, D. K.; et al, Green, D. W. E. , 编, V4332 Sagittarii, IAU Circular, August 2006, 8739 (1): 1, Bibcode:2006IAUC.8739....1L.
Banerjee, Dipankar P. K., Studies of the peculiar nova V4332 Sgr, Bulletin of the Astronomical Society of India, June 2005, 33 (2): 81, Bibcode:2005BASI...33...81B.
Banerjee, Dipankar P. K.; et al, L and M Band Infrared Studies of V4332 Sagittarii: Detection of the Water Ice Absorption Band at 3.05 μm and the CO Fundamental Band in Emission, The Astrophysical Journal, November 2004, 615 (1): L53–L56, Bibcode:2004ApJ...615L..53B, S2CID 119099260, arXiv:astro-ph/0409393 , doi:10.1086/425963.
Banerjee, Dipankar P. K.; et al, A Search for Radioactive 26Al in the Nova-like Variable V4332 Sagittarii, The Astrophysical Journal, July 2004, 610 (1): L29–L32, Bibcode:2004ApJ...610L..29B, S2CID 119073232, arXiv:astro-ph/0406453 , doi:10.1086/423171.
Banerjee, Dipankar P. K.; Ashok, Nagarhalli M., Optical Studies of V4332 Sagittarii: Detection of Unusually Strong K I and Na I Lines in Emission, The Astrophysical Journal, March 2004, 604 (1): L57–L60, Bibcode:2004ApJ...604L..57B, S2CID 119424917, arXiv:astro-ph/0406452 , doi:10.1086/383264.
Banerjee, Dipankar P. K.; et al, Remarkable Changes in the Near-Infrared Spectrum of the Nova-like Variable V4332 Sagittarii, The Astrophysical Journal, November 2003, 598 (1): L31–L34, Bibcode:2003ApJ...598L..31B, S2CID 123386138, arXiv:astro-ph/0310088 , doi:10.1086/380389.