论文标题
级别0低质量原始原始源IRAS IRAS 16293-2422源A的子结构在10 AU量表上a
Substructures in the Disk-Forming Region of the Class 0 Low-Mass Protostellar Source IRAS 16293-2422 Source A on a 10 au Scale
论文作者
论文摘要
我们已经观察到C17O和H2CS线中的0类Protostellar Source IRAS 16293-2422 A以及与Atacama大毫米/亚毫升阵列的1.3 mm尘埃连续性，其角度分辨率为〜0。 Protostar。以300个AU的尺度以连续体的强度为中心，而在50 au的半径内，圆形的结构却是较小的，相比之下在A1周围的磁盘。我们使用多个H2C的线来得出旋转，旋转温度陡峭地上升到300 K或更高的速度。据报道，由于H2C的旋转温度的升高最有可能代表气体和灰尘温度的升高，有机分子线被增强。
We have observed the Class 0 protostellar source IRAS 16293-2422 A in the C17O and H2CS lines as well as the 1.3 mm dust continuum with the Atacama Large Millimeter/submillimeter Array at an angular resolution of ~0."1 (14 au). The continuum emission of the binary component, Source A, reveals the substructure consisting of 5 intensity peaks within 100 au from the protostar. The C17O emission mainly traces the circummultiple structure on a 300 au scale centered at the intensity centroid of the continuum, while it is very weak within the radius of 50 au from the centroid. The H2CS emission, in contrast, traces the rotating disk structure around one of the continuum peaks (A1). Thus, it seems that the rotation centroid of the circummultiple structure is slightly different from that of the disk around A1. We derive the rotation temperature by using the multiple lines of H2CS. As approaching to the protostar A1, the rotation temperature steeply rises up to 300 K or higher at the radius of 50 au from the protostar. It is likely due to a local accretion shock and/or the preferential protostellar heating of the transition zone from the circummultiple structure to the disk around A1. This position corresponds to the place where the organic molecular lines are reported to be enhanced. Since the rise of the rotation temperature of H2CS most likely represents the rise of the gas and dust temperatures, it would be related to the chemical characteristics of this prototypical hot corino.
