Luminous Red Nova 2015 in the Galaxy M101
Luminous Red Nova 2015 in the Galaxy M101
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Galaxy M101 中的夜光红色 Nova 2015
DOI：
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发表时间：
2016
期刊：
影响因子：
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通讯作者：
T. Hancock
中科院分区：
文献类型：
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作者：
V. Goranskij;E. Barsukova;O. Spiridonova;A. Valeev;T. Fatkhullin;A. Moskvitin;O. Vozyakova;D. Cheryasov;B. Safonov;A. Zharova;T. Hancock
我们提出了基于俄罗斯6米望远镜（BTA）以及SAO RAS和SAI MSU的其他望远镜进行的观测的红新星PSN J140216 78+5426205的研究结果。为了研究无尾星的祖先，我们使用了数字巡天的数据和互联网上的业余照片。在1993年4月至2014年7月期间，祖星的亮度逐渐增加了2。i’我在他们的乐队里。在2014年11月中旬第一次爆发的高峰期，这颗恒星的绝对视星等达到了- 12。m75，但后来在2015年2月被发现，在一次绝对星等为- 11的重复爆发中。m65。突出幅度在赤霞星中最小，只有5个。在他们的v波段。在光谱中观测到Hα发射线和表面温度逐渐降低的冷超巨星连续体。这一过程在红新星中是典型的，尽管我们所研究的天体显示出极端的参数：最大亮度、最大爆发持续时间、最小爆发幅度、不寻常的光曲线形状。这一事件被解释为一个巨大的OB恒星系统的组成部分的合并伴随着一个共同的包层的形成，然后这个包层的膨胀以最小的能量损失。
We present the results of the study of the red nova PSN J140216 78+5426205 based on the observations carried out with the Russian 6-m telesco pe (BTA) along with other telescopes of SAO RAS and SAI MSU. To investigate the no va progenitor, we used the data from the Digital Sky Survey and amateur photos a vailable on the internet. In the period between April 1993 and July 2014, the brigh tness of the progenitor gradually increased by 2 . m in theV band. At the peak of the first outburst in midNovember of 2014, the star reached an absolute visual magnit ude of−12. m75 but was discovered later, in February 2015, in a repeated outburst a t the absolute magnitude of −11. m65. The amplitude of the outburst was minimum among the red no vae, only 5. m6 in theV band. The Hα emission line and the continuum of a cool supergiant with a gradually decreasing surface temperature were obser ved in the spectra. Such process is typical for red novae, although the object under s tudy showed extreme parameters: maximum luminosity, maximum outburst duratio n, minimum outburst amplitude, unusual shape of the light curve. This event is in terpreted as a massive OB star system components’ merging accompanied by the forma tion of a common envelope and then the expansion of this envelope with minima l energy losses.