ECLIPSES DURING THE 2010 ERUPTION OF THE RECURRENT NOVA U SCORPII
ECLIPSES DURING THE 2010 ERUPTION OF THE RECURRENT NOVA U SCORPII
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2010 年天蝎座新星爆发期间的日食
DOI：
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发表时间：
2011
期刊：
影响因子：
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通讯作者：
M. Shara
中科院分区：
文献类型：
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作者：
B. Schaefer;A. Pagnotta;A. Lacluyze;D. Reichart;K. Ivarsen;J. Haislip;M. Nysewander;J. Moore;A. Oksanen;H. Worters;R. Sefako;J. Mentz;S. Dvorak;T. Gomez;B. Harris;A. Henden;T. Tan;M. Templeton;W. Allen;B. Monard;R. Rea;G. Roberts;W. Stein;H. Maehara;T. Richards;C. Stockdale;T. Krajci;G. Sjoberg;J. McCormick;M. Revnivtsev;S. Molkov;V. Suleimanov;M. Darnley;M. Bode;G. Handler;S. Lépine;M. Shara
在2010年1月28日，天蝎座U的爆发是有史以来观测到的最好的新星事件。我们在67天的喷发中报告了36，776级，平均每2.6分钟测量一次。这种独特的和前所未有的覆盖范围是第一次，一颗新星有任何实质性的快速测光。有了这个，两个新的现象被发现：在第9-15天看到的早期光变曲线中的快速耀斑（没有提出解释）和在第41-61天看到的日食中的光学下降（可能是由吸积盘的凸起边缘掩盖了盘的明亮内部区域引起的，如在特定的轨道相位上看到的）。膨胀的壳层和风在第12-15天变得足够清晰，因此内部的双星系统变得可见，导致日食的突然发生和超软X射线源的开启。在第15天，食外光线的强烈不对称性表明吸积流的存在。正常的光学闪烁在第24.5天重新开始。在第15-26天，日食映射显示光源是球对称的，半径为4.1 R。对于第26-41天，可见光来自半径为3.4 R的边缘明亮盘。对于第41-67天，光源是半径为2.2 R的中心明亮盘。在整个喷发过程中，颜色基本保持不变。我们在喷发期间提供了12次日食，加上喷发后的5次。
The eruption of the recurrent nova U Scorpii on 2010 January 28 is now the all-time best observed nova event. We report 36,776 magnitudes throughout its 67 day eruption, for an average of one measure every 2.6 minutes. This unique and unprecedented coverage is the first time that a nova has had any substantial amount of fast photometry. With this, two new phenomena have been discovered: the fast flares in the early light curve seen from days 9–15 (which have no proposed explanation) and the optical dips seen out of eclipse from days 41–61 (likely caused by raised rims of the accretion disk occulting the bright inner regions of the disk as seen over specific orbital phases). The expanding shell and wind cleared enough from days 12–15 so that the inner binary system became visible, resulting in the sudden onset of eclipses and the turn-on of the supersoft X-ray source. On day 15, a strong asymmetry in the out-of-eclipse light points to the existence of the accretion stream. The normal optical flickering restarts on day 24.5. For days 15–26, eclipse mapping shows that the optical source is spherically symmetric with a radius of 4.1 R☉. For days 26–41, the optical light is coming from a rim-bright disk of radius 3.4 R☉. For days 41–67, the optical source is a center-bright disk of radius 2.2 R☉. Throughout the eruption, the colors remain essentially constant. We present 12 eclipse times during eruption plus five just after the eruption.