arXiv 1909.061452019-09-13astro-ph.GA

麒麟座OB 1恒星形成区的多尺度分析：II。麒麟座OB1分子云中的碰撞细丝

Multi-scale analysis of the Monoceros OB 1 star-forming region: II. Colliding filaments in the Monoceros OB1 molecular cloud

Julien Montillaud, Mika Juvela, Charlotte Vastel, J. H. He, Tie Liu, Isabelle Ristorcelli, David J. Eden, Sung-ju Kang, Kee-Tae Kim, Patrick M. Koch, Chang Won … 展开作者

Julien Montillaud, Mika Juvela, Charlotte Vastel, J. H. He, Tie Liu, Isabelle Ristorcelli, David J. Eden, Sung-ju Kang, Kee-Tae Kim, Patrick M. Koch, Chang Won Lee, Mark G. Rawlings, Mika Saajasto, Patricio Sanhueza, Archana Soam, Sarolta Zahorecz, Dana Alina, Rebeka Bögner, David Cornu, Yasuo Doi, Johanna Malinen, Douglas Marshall, E. R. Micelotta, V. M. Pelkonen, L. V. Tóth, A. Traficante, Ke Wang

备注：: A&A, in press; IRAM and TRAO data cubes will be available at CDS
发表信息：: A&A 631, A3 (2019)
DOI：: 10.1051/0004-6361/201834903

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摘要：

我们开始对G202.3+2.5进行多尺度分析，这是Monoceros OB 1的一个交织的附属区域。在第一篇论文中，我们研究了致密核和原恒星的分布，并发现在暗条的连接区有增强的恒星形成（SF）活动。在这第二篇论文中，我们的目标是揭示核心和细丝演化之间的联系，以及细丝动力学和云的全球演化之间的联系。我们利用Herschel和WISE观测以及IRAM 30 m和TRAO 14 m望远镜观测到的分子示踪剂，对气体动力学和能量平衡进行了研究。云的速度场进行了检查和速度相干结构与云环境的角度。两个主要的速度分量（VC）被发现，以及分离的北部和合并的位置附近的强烈N2 H+排放的文件我发现SF活动的峰值。两个VC沿视线的相对位置以及N2 H+发射的速度梯度表明VC已经经历了约10^5年的碰撞。检测到N2 H+的稠密气体被解释为两个细丝之间的压缩区域，这对应于约1 e-3 Msun/yr的高质量流入速率，并可能导致其SF效率的增加。我们确定了一个原恒星的交界区，可能权力两个交叉间歇性流出。我们发现，附近的集群NCG 2264周围的HII区域仍在扩大，并检查其在碰撞中的作用。然而，我们不能排除碰撞主要来自云的全球崩溃的想法。本文研究的（子）尺度观测值揭示了G202.3+2.5子结构之间的碰撞及其在结区核心馈电中的可能作用。我们现在必须以高解析度观测云的形态、碎片和磁场。

英文摘要：

We started a multi-scale analysis of G202.3+2.5, an intertwined filamentary region of Monoceros OB1. In Paper I, we examined the distributions of dense cores and protostars and found enhanced star formation (SF) activity in the junction region of the filaments. In this second paper, we aim to unveil the connections between the core and filament evolutions, and between the filament dynamics and the global evolution of the cloud. We characterise the gas dynamics and energy balance using Herschel and WISE observations and molecular tracers observed with the IRAM 30m and TRAO 14m telescopes. The velocity field of the cloud is examined and velocity-coherent structures are put in perspective with the cloud environment. Two main velocity components (VCs) are revealed, well separated in the north and merged around the location of intense N2H+ emission where Paper I found the peak of SF activity. The relative position of the two VCs along the sightline, and the velocity gradient in N2H+ emission imply that the VCs have been undergoing collision for ~10^5 yrs. The dense gas where N2H+ is detected is interpreted as the compressed region between the two filaments, which corresponds to a high mass inflow rate of ~1e-3 Msun/yr and possibly leads to an increase in its SF efficiency. We identify a protostar in the junction region that possibly powers two crossed intermittent outflows. We show that the HII region around the nearby cluster NCG 2264 is still expanding and its role in the collision is examined. However, we cannot rule out the idea that the collision arises mostly from the global collapse of the cloud. The (sub-)filament-scale observables examined in this paper reveal a collision between G202.3+2.5 sub-structures and its probable role in feeding the cores in the junction region. One must now characterise the cloud morphology, its fragmentation, and magnetic field, all at high resolution.

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英文摘要：

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