1995年至2006年期间爆发的年轻恒星OO Serpentis的爆发
The outburst of the eruptive young star OO Serpentis between 1995 and 2006
摘要：
巨蛇座OO是一颗深埋的前主序星，于1995年爆发，之后逐渐褪色。它的爆发类似于著名的FU Orionis型或EX Lupi型爆发。由于很少有这样的事件曾经被记录在红外波长，我们的目标是研究的时间演变OO Ser在红外。OO Ser由红外空间天文台监测，从亮度峰值后4个月开始，持续20个月。在2004-2006年，我们再次从地面观测到OO Ser，并补充了2004年斯皮策观测数据集。我们分析了这些数据，特别注意源混淆，并在10个不同的波长以及光谱能量分布的光变曲线。这次爆发使整个红外区域都变亮了。根据红外线曲线，OO Ser在峰值亮度之后开始与波长无关的衰减。后来，通量衰减变慢，但保持波长无关。衰落仍在继续，目前的衰落率表明OO Ser在2011年之前不会恢复到静止状态。OO Ser的爆发时间尺度似乎比FUors短，但比EXors长。爆发的时间尺度和中等的光度表明OO Ser不同于FUors和EXors，并且与最近爆发的年轻恒星V1647 Ori相似。根据它的光谱能量分布和测热温度，OO Ser似乎是一个早期的I类天体，年龄小于10^5年。该天体可能被一个吸积盘和一个致密的包层所包围。由于较短的爆发时间尺度，在拱盘OO Ser的粘度可能是一个数量级高于通常的FUors。
英文摘要：
OO Serpentis is a deeply embedded pre-main sequence star that went into outburst in 1995 and gradually faded afterwards. Its eruption resembled the well-known FU Orionis-type or EX Lupi-type outbursts. Since very few such events have ever been documented at infrared wavelengths, our aim is to study the temporal evolution of OO Ser in the infrared. OO Ser was monitored with the Infrared Space Observatory starting 4 months after peak brightness and covering 20 months. In 2004-2006 we again observed OO Ser from the ground and complemented this dataset with archival Spitzer obsevations also from 2004. We analysed these data with special attention to source confusion and constructed light curves at 10 different wavelengths as well as spectral energy distributions. The outburst caused brightening in the whole infrared regime. According to the infrared light curves, OO Ser started a wavelength-independent fading after peak brightness. Later the flux decay became slower but stayed wavelength-independent. The fading is still ongoing, and current fading rates indicate that OO Ser will not return to quiescent state before 2011. The outburst timescale of OO Ser seems to be shorter than that of FUors, but longer than that of EXors. The outburst timescale and the moderate luminosity suggest that OO Ser is different from both FUors and EXors, and shows similarities to the recently erupted young star V1647 Ori. Based on its spectral energy distribution and bolometric temperature, OO Ser seems to be an early class I object, with an age of < 10^5 yr. The object is probably surrounded by an accretion disc and a dense envelope. Due to the shorter outburst timescales, the viscosity in the circumstellar disc of OO Ser is probably an order of magnitude higher than usual for FUors.
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