A BUBBLING NEARBY MOLECULAR CLOUD: COMPLETE SHELLS IN PERSEUS
A BUBBLING NEARBY MOLECULAR CLOUD: COMPLETE SHELLS IN PERSEUS
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DOI：
10.1088/0004-637x/742/2/105
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发表时间：
2011-09
期刊：
影响因子：
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通讯作者：
H. Arce;M. Borkin;A. Goodman;J. Pineda;Christopher Beaumont
中科院分区：
文献类型：
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作者：
H. Arce;M. Borkin;A. Goodman;J. Pineda;Christopher Beaumont
我们用完整的12CO(1-0)和13CO(1-0)图研究了英仙座分子云中的壳层(和气泡)。这里报告的12个贝壳分布在英仙座星云的大部分地区，具有圆形或弧形的形态，半径范围约为0.1-3pC。其中大多数以前没有被发现，很可能是因为该地区的地图缺乏区分它们所需的复盖面和分辨率。大多数贝壳与形状相似的红外星云重合，并在中心附近有一个候选动力源。我们认为，它们是由英仙座分子云内部或附近的年轻恒星提供动力的球状或极大角风的相互作用形成的-英仙座分子云通常被认为形成了主要是低质量的恒星。12个外壳中有两个由靠近云层的大质量恒星提供动力，而其他外壳似乎由云中的低质量或中等质量恒星提供动力。我们认为，产生观测到的贝壳需要质量损失率约为10−8到10−6 M☉yr−1的风。我们的估计表明，这些恒星风的能量输入率与湍流耗散率相似。我们的结论是，在英仙座，来自准直的原恒星外流和来自年轻恒星的强大球面风的总能量输入足以维持分子云中的湍流。云层样本的大尺度分子线和红外连续谱图将有助于确定这种现象在其他恒星形成区域的频率。
We present a study of the shells (and bubbles) in the Perseus molecular cloud using the COMPLETE survey large-scale 12CO(1–0) and 13CO(1–0) maps. The 12 shells reported here are spread throughout most of the Perseus cloud and have circular or arc-like morphologies with a range in radius of about 0.1–3 pc. Most of them have not been detected before most likely because maps of the region lacked the coverage and resolution needed to distinguish them. The majority of the shells are coincident with infrared nebulosity of similar shape and have a candidate powering source near the center. We suggest that they are formed by the interaction of spherical or very wide angle winds powered by young stars inside or near the Perseus molecular cloud—a cloud that is commonly considered to be forming mostly low-mass stars. Two of the 12 shells are powered by high-mass stars close to the cloud, while the others appear to be powered by low- or intermediate-mass stars in the cloud. We argue that winds with a mass loss rate of about 10−8 to 10−6 M☉ yr−1 are required to produce the observed shells. Our estimates indicate that the energy input rate from these stellar winds is similar to the turbulence dissipation rate. We conclude that in Perseus the total energy input from both collimated protostellar outflows and powerful spherical winds from young stars is sufficient to maintain the turbulence in the molecular cloud. Large-scale molecular line and IR continuum maps of a sample of clouds will help determine the frequency of this phenomenon in other star-forming regions.