The 2010 outburst and pre-outburst optical spectrum of the recurrent nova U Scorpii
The 2010 outburst and pre-outburst optical spectrum of the recurrent nova U Scorpii
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复发新星天蝎座 U 2010 年爆发和爆发前的光谱
DOI：
10.1051/0004-6361/201321262
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发表时间：
2013
影响因子：
6.5
通讯作者：
Anupama G
中科院分区：
文献类型：
--
作者：
Anupama G
目的研究2010年复发新星天蝎座U爆发期间的演化过程。方法在爆发极大值后0.83-162.5天内获得了该新星的光谱观测资料。光学线性偏振观测之前的超软X射线源（SSS）阶段和SSS阶段期间的发病。无线电连续观测是在1280 MHz波段的早期下降阶段，并在610 MHz波段的SSS阶段的开始和结束。我们还提出了在爆发前的quiescence phase.ResultsThe整体光谱演化在2010年的爆发是类似于以前的爆发。然而，密集的时间覆盖，特别是在早期阶段，揭示了一些短期的变化，以前没有报道。早期阶段的发射线的宽度表明非常高的速度为新星喷出物，~10 000公里s-1。线条轮廓宽阔，四四方方，结构严谨。在6.83天的光谱中，观测到了与He I谱线有关的窄的P-Cygni散射，其速度约为500 km/s，同时还观测到了Ca II、NI和氢谱线（波长>8000 nm），这些谱线是在一次光学耀斑之后立即获得的。这种吸收成分可能是在等离子体中产生的，这些等离子体发射出X射线中看到的氮线，可能位于双星轨道之外。在4660 N III特征的强度中检测到快速变化，这表明在第8.83天和第13.82天，在轨道相位分别为0.75和0.25时，线强度显着增加。就在发病前和SSS阶段期间检测到固有极化，SSS阶段期间pv约为1.4%。的N III功能和内在极化的通量变化是最有可能与重整吸积盘/流。对于球壳几何形状，我们估计喷射出的（氢）壳的质量约为4.6 × 10- 6 M Ω。在1280 MHz和610 MHz的无线电波段中没有探测到U Sco，这与新星喷出物的低质量、次级的亚巨星性质以及到新星的距离是一致的。
AimsWe study the evolution of the recurrent nova U Scorpii during its outburst in 2010.MethodsOptical spectroscopic observations of the nova were obtained during 0.83–162.5 days after outburst maximum. Optical linear polarisation observations were made before the onset of the super soft X-ray source (SSS) phase and during the SSS phase. Radio continuum observations were made in the 1280 MHz band during the early decline phase, and in the 610 MHz band at the onset and end of the SSS phase. We also present optical spectra obtained in the pre-outburst quiescence phase.ResultsThe overall spectral evolution during the 2010 outburst is similar to the previous outbursts. However, the dense temporal coverage, especially during the early phases, reveals several short term variations not reported previously. The early phase emission line widths indicate extremely high velocities for the nova ejecta, ~10 000 km s-1. The line profiles are broad, boxy and structured. Narrow P-Cygni absorptions, at ~500 km s-1are seen associated with the He I lines, and also the Ca II, N I and hydrogen lines (at wavelengths >8000 Å) in the spectrum of day 6.83, obtained immediately after an optical flare. This absorption component could be arising in the plasma emitting the Nitrogen lines seen in X-rays, that probably lies outside the binary orbit. Rapid variations are detected in the strength of the 4660 Å N III feature, which shows a significant increase in the line strength on days 8.83 and 13.82, at orbital phases of 0.75 and 0.25, respectively. Instrinsic polarisation is detected just before the onset, and during the SSS phase, withpv~ 1.4% during the SSS phase. The flux variations of the N III feature and the intrinsic polarisation are most likely associated with the reforming accretion disc/stream. We estimate the mass of the ejected (hydrogen) shell to be ~4.6 × 10-6M⊙, for a spherical shell geometry. The non-detection of U Sco in the 1280 MHz and 610 MHz radio bands is consistent with the low mass of the nova ejecta, subgiant nature of the secondary, and the distance to the nova.
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期刊：
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2011
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发表时间：
2011
期刊：
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发表时间：
2010
期刊：
影响因子：
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A. Pagnotta;B. Schaefer;G. Handler;W. Allen;T. Campbell;T. Krajci;B. Monard;R. Rea;T. Richards;G. Roberts;William Stein;C. Stockdale;J. McCormick;S. Dvorak;T. Gomez;B. Harris;A. Henden;G. Sjoberg;T. Tan;A. Oksanen
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