V1647 Orionis (IRAS 05436−0007) in Outburst: The First Three Months
V1647 Orionis (IRAS 05436−0007) in Outburst: The First Three Months
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V1647 Orionis (IRAS 05436−0007) 爆发：前三个月
DOI：
10.1086/423703
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发表时间：
2004
期刊：
影响因子：
--
通讯作者：
Angeliki Field
中科院分区：
文献类型：
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作者：
F. Walter;G. Stringfellow;W. Sherry;Angeliki Field
我们报告的光度（BVRIJHK）和低色散光谱观测猎户座V1647，星星，驱动麦克尼尔星云，2004年2月10日和5月7日之间。这颗星星在这87天中光度变化很大，亮度一般下降约0.3-0.4等。除了Hα和Ca II红外三重态发射和Na II D吸收特征外，光谱没有特征。Ca II三重线比率是典型的年轻恒星天体。Hα等效宽度可在约60天的周期内进行调制。爆发后的灭绝似乎是小于7马格。这些数据是一个FU猎户座类事件的暗示，但需要进一步的监测，以明确的特点爆发。
We report on photometric (BVRIJHK) and low-dispersion spectroscopic observations of V1647 Orionis, the star that drives McNeil's Nebula, between 2004 February 10 and May 7. The star is photometrically variable atop a general decline in brightness of about 0.3–0.4 mag during these 87 days. The spectra are featureless, aside from Hα and the Ca II infrared triplet in emission and a Na II D absorption feature. The Ca II triplet line ratios are typical of young stellar objects. The Hα equivalent width may be modulated on a period of about 60 days. The postoutburst extinction appears to be less than 7 mag. The data are suggestive of an FU Orionis–like event, but further monitoring will be needed to definitively characterize the outburst.