船尾座V445

船尾座V445

船尾座V445的双极壳层喷射从2005年（左上）到2007年（右下）不断增强。
Credit: ESO/P.A. Woudt
觀測資料
曆元 J2000
星座 船尾座
星官
赤經 07h 37m 56.90s[1]
赤緯 –25° 56′ 58.9″[1]
視星等（V）
天体测定
距离27,000[2] ly
(8,200 pc)
詳細資料
金屬量

船尾座V445是一颗位于船尾座的新星。它由金津和义于2000年11月28日在日本松江市发现，当时它的视星等正达到最大值8.6。2000年12月30日，京都大学的加藤太一在国际天文学联合会第7552号通报中报告了这颗新星[3]。这颗新星的位置与1967年就已拍摄到的一颗13.1等的恒星相符。此恒星的自行速度测量值为赤经方向-4.7 角分/年，赤纬方向+6.4 角分/年，测量结果的标准差为4 角分/年[4]。

光谱

对该新星的光谱分析表明它存在钙（Ca I）、钠（Na I）和单电离的铁（Fe II）的吸收谱线。初始瞬态吸收谱表明含氢很少，不符合其他典型新星的光谱的类型[4][5]。次年1月31日的红外光谱实验发现很普通的连续谱减少，同时波长增大。这与受热尘埃的喷射相符，表明这是一颗再发新星，在爆发之前先喷射尘埃[6]。到2004年，此天体变回正常亮度，尘埃喷发现象也消失了[7]。

这次爆发中氢的含量很少，而氦和碳的含量却反常地多。这些事实与电离程度较高一起表明，这是第一颗观测到的氦新星。理论上来说，氦新星是因为白矮星从环绕的伴星中获得的氦比氢更多。当白矮星表面的壳层累积了充足的氦时，就会发生一次对外抛射物质的新星热核爆炸。因此，船尾座V445可能是一个双星系统，周围围绕的吸积盘是从伴星获得的物质[8]。

现状

目前，这个系统隐藏在一个很厚的光学尘埃云后方[2]，并观测到一股双极喷流物质正以6,720±650 km/s的速度离开这个系统。喷流中物质的结节正在以8,450±570 km/s的高速运动。根据喷流不断扩大的视差，此系统离我们的距离为8.2±0.5 千秒差距[9]。

船尾座V445系统中的白矮星估计质量可超过太阳质量的1.3倍，而且在不断增加。这是因为再发的氦壳层会反射吸积的物质。当这颗白矮星的质量超过大约1.38倍太阳质量的钱德拉塞卡极限时，它将可能成为一颗Ia型超新星[2]。

参考资料

  1. ^ 1.0 1.1 V* V445 Pup -- Nova. SIMBAD. Centre de Données astronomiques de Strasbourg. [2010-03-02]. 
  2. ^ 2.0 2.1 2.2 Kato, Mariko; Hachisu, Izumi; Kiyota, Seiichiro; Saio, Hideyuki. Helium Nova on a Very Massive White Dwarf: A Revised Light-Curve Model of V445 Puppis (2000). The Astrophysical Journal. September 2008, 684 (2): 1366–1373. Bibcode:2008ApJ...684.1366K. doi:10.1086/590329. 
  3. ^ Circular No. 7552. IAU. [2011-07-05]. （原始内容存档于2012-05-01）. 
  4. ^ 4.0 4.1 Circular No. 7556. IAU. [2011-07-05]. （原始内容存档于2012-05-01）. 
  5. ^ Ashok, N. M. Infrared study of the first identified helium nova V445 Puppis. Bulletin of the Astronomical Society of India. June 2005, 33 (2): 75–79. Bibcode:2005BASI...33...75A. 
  6. ^ Circular No. 7580. IAU. [2011-07-05]. （原始内容存档于2012-05-01）. 
  7. ^ Circular No. 8642. IAU. [2011-07-05]. （原始内容存档于2012-05-01）. 
  8. ^ Ashok, N. M.; Banerjee, D. P. K. The enigmatic outburst of V445 Puppis - A possible helium nova?. Astronomy and Astrophysics. October 2003, 409: 1007–1015. Bibcode:2003A&A...409.1007A. arXiv:astro-ph/0307304 可免费查阅. doi:10.1051/0004-6361:20031160. 
  9. ^ Woudt, P. A.; et al.. The Expanding Bipolar Shell of the Helium Nova V445 Puppis. The Astrophysical Journal. November 2009, 706 (1): 738–746. Bibcode:2009ApJ...706..738W. doi:10.1088/0004-637X/706/1/738. 

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