L183的BIMA N2H + 1-0映射观测--坍缩、磁化、旋转、前星核中的碎裂和自旋
BIMA N2H+ 1-0 mapping observations of L183 -- fragmentation and spin-up in a collapsing, magnetized, rotating, pre-stellar core
摘要：
为了研究L183星核致密部分的空间和运动学亚结构，我们利用伯克利-伊利诺伊-马里兰阵列（BIMA）对L183星核进行了N2 H + 1-0的深度成像。检测到三个空间和运动学上不同的团块，我们将其标记为L183-N1、L183-N2和L183-N3。L183-N2与亚毫米级尘埃峰值大致重合，位于L183的系统速度处。因此，我们认为L183-N2是L183的中心致密核。L183-N1和L183-N3是新发现的L183碎片，其速度梯度与L183整体的速度梯度平行，但远强于L183整体的速度梯度。此外，大尺度和小尺度的速度梯度的比率，以及它们各自的尺寸尺度的比率，与旋转的角动量守恒是一致的，坍缩的核心经历自旋。推断出的旋转轴平行于磁场方向，与我们在其他前星核中看到的一样，磁场方向偏离了长轴。因此，我们提出，我们已经检测到一个破碎的，崩溃的，无意识的，前恒星的核心，围绕它的B场旋转，这是旋转，因为它的崩溃。它可能会继续形成一个多原恒星系统。
英文摘要：
We have used the Berkeley-Illinois-Maryland Array (BIMA) to make deep N2H+ 1-0 maps of the pre-stellar core L183, in order to study the spatial and kinematic substructure within the densest part of the core. Three spatially and kinematically distinct clumps are detected, which we label L183-N1, L183-N2 and L183-N3. L183-N2 is approximately coincident with the submillimetre dust peak and lies at the systemic velocity of L183. Thus we conclude that L183-N2 is the central dense core of L183. L183-N1 and 3 are newly-discovered fragments of L183, which are marked by velocity gradients that are parallel to, but far stronger than, the velocity gradient of L183 as a whole, as detected in previous single-dish data. Furthermore, the ratio of the large-scale and small-scale velocity gradients, and the ratio of their respective size-scales, are consistent with the conservation of angular momentum for a rotating, collapsing core undergoing spin-up. The inferred axis of rotation is parallel to the magnetic field direction, which is offset from its long axis, as we have seen in other pre-stellar cores. Therefore, we propose that we have detected a fragmenting, collapsing, filamentary, pre-stellar core, rotating about its B-field, which is spinning up as it collapses. It will presumably go on to form a multiple protostellar system.
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