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首页> 外文期刊>The Astrophysical journal >MASS LOSS AND JET OUTFLOW IN THE ORION NEBULA PROPLYD LV 2
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MASS LOSS AND JET OUTFLOW IN THE ORION NEBULA PROPLYD LV 2

机译：Orion Nebula提供的LV 2中的质量损失和射流流出

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摘要

We have obtained Hubble Space Telescope (HST) Space Telescope Imaging Spectrometer high-resolution spectra of the Orion proplyd LV 2 in the C Ⅲ doublet at 1906.68 and 1908.73 A. New images at the 6 cm wavelength with MERLIN complement earlier HST images at a similar spatial resolution. This object is one of the closest proplyds to θ~1 Ori C, the source of the photoionizing and photoevapo-rating radiation. Combining the spectra with the HST images and detailed theoretical models has allowed a determination of the mass-loss rate as 8.2 x 10~(-7) solar mass yr~(-1) +- 10%. This rate of mass loss is used to address the conundrum of the continued existence of proplyds. Even though they should be photoevaporated in only about 10~5 yr, there is no evidence for their destruction. It is concluded that the only explanation is that the age of θ~1 Ori C is less than 10~5 yr. These spectra and previously unpublished ground-based spectra in [O Ⅲ] also show the presence of a monopolar microjet, redshifted by about 100 km s~(-1) with respect to the systemic velocity. This jet is more visible in the 6 cm MERLIN images than in HST images, and this image together with the spectra are used to determine the flow parameters for the jet. Our spectra also include the stand-off shock that lies between LV 2 and θ~0 Ori C. This is the result of the high-velocity wind coming from the hot star θ~1 Ori C with the low-velocity wind coming from the proplyd. As expected, this shock is at rest with respect to the two objects.
机译：我们已经获得了哈勃太空望远镜（HST）太空望远镜成像光谱仪在1906.68和1908.73 A处CⅢ双峰中猎户座LV 2的高分辨率光谱。使用MERLIN在6 cm波长处的新图像以类似的方式补充了较早的HST图像。空间分辨率。该物体是θ〜1 Ori C（光电离和光蒸发辐射的来源）的最接近的物体之一。将光谱与HST图像和详细的理论模型相结合，可以确定质量损失率为8.2 x 10〜（-7）太阳质量yr〜（-1）+-10％。这种质量损失率用于解决脯氨酸持续存在的难题。即使仅在约10〜5年内将它们蒸发，也没有证据表明它们会被破坏。结论是，唯一的解释是θ〜1 Ori C的年龄小于10〜5 yr。这些光谱和以前未发表的[OⅢ]地基光谱也表明存在单极微射流，它相对于系统速度红移了约100 km s〜（-1）。在6 cm MERLIN图像中，此喷射比在HST图像中更明显，并且此图像与光谱一起用于确定喷射的流量参数。我们的频谱还包括位于LV 2和θ〜0 Ori C之间的对峙冲击。这是来自热恒星θ〜1 Ori C的高速风和来自恒星的低速风的结果。提议。不出所料，这种冲击相对于两个物体是静止的。

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