人马座V4332
|-
| 观测资料 历元 J2000.0 | |
|---|---|
| 星座 | 人马座 |
| 星官 | |
| 赤经 | 18h 50m 36.696s[3] |
| 赤纬 | –21° 23′ 28.93″[3] |
| 视星等（V） | 8.5[2] |
| 特性 | |
| 光谱分类 | K8/M0e[4] |
| 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[3] mas |
| 距离 | (3.71±3.3)×103[5] ly |
| 其他命名 | |
V4332 Sgr、Nova Sgr 1994[6]
| |
| 参考数据库 | |
| SIMBAD | 资料 |
人马座V4332是在星座人马座中类似新星事件。它于1994年2月24日由在日本爱知冈崎的业余天文学家山本实（Minoru Yamamoto）发现，视星等为8.9等，随后由广泽（K.Hirosawa）证实[7]。最初命名为新星人马座1994#1，并依据变星命名法命名为人马座[2]。3月4日拍摄的事件的光谱缺乏经典新星的特征，唯一的发射线是氢光谱的巴耳末系[8]。随后的光谱显示光度在五天内迅速下降，光谱类型发生变化[2]。到2003年，该天体的亮度比峰值时的星等低约1,500倍，并显示出M型恒星的光谱[9]。
类似新星的事件麒麟座V838和这次爆发形成了一类不同寻常的喷发恒星。2003年，N.Soker和R.Tylenda提出了一个吸积的场景作为解释。他们指出，在一个封闭的双星轨道上合并两颗主序星可以解释观测到的性质[10]，这一过程现在被称为亮红新星。在这种情况下，人马座V4332的亮度和半径的下降是合并后的恒星外壳经历引力收缩的结果[9]。
来自该物体的红外过量表明它有一个星周盘。该特征的红外光谱显示出水冰的吸收带和一氧化碳发射带[9]。到2010年，恒星成分已经被边缘观察到的尘土飞扬的圆盘所掩盖[1]。这种灰尘的重要成分包括氧化铝，与含量不断增加的氧化镁和氧化铁[11]。
相关条目[编辑]
参考资料[编辑]
- ^ 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] 请检查
|url=值 (帮助). SIMBAD. 斯特拉斯堡天文资料中心. - ^ 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.
进阶读物[编辑]
- 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.