SNR撞击磁化中性云引发的恒星形成
Star formation triggered by SNR impact into magnetized neutral clouds
摘要：
考虑到物理条件是相关的触发恒星形成的相互作用，涉及SN冲击和中性云，我们已经建立了图的SNR半径与云密度，这些条件约束的阴影区，恒星形成是允许的。图还测试与全3-D MHD辐射冷却模拟涉及SNR和自引力云，我们发现，数值分析是一致的，由图预测的结果。虽然包含一个近似垂直于SNR的撞击速度的均匀磁场，其强度为~1 $mu$ G，但图中的恒星形成区仅会出现小幅收缩，而更大的磁场（~10 $μ$ G）会导致显著收缩，正如预期的那样。我们的研究结果在我们自己的星系中的真正的恒星形成区域的应用表明，它们的形成可能是由SN冲击波触发的。最后，我们评估了这种相互作用的有效全球恒星形成效率，发现它小于我们银河系的观测值（SFE ~0.01-0.3）。这一结果与文献中以前的工作是一致的，也表明目前研究的机制，虽然非常强大的驱动结构形成，超音速湍流，并最终，本地恒星形成，似乎不足以驱动全球恒星形成在正常的恒星形成星系。
英文摘要：
Considering the physical conditions that are relevant for triggering star formation in interactions involving SN shocks and neutral clouds, we have built diagrams of the SNR radius versus the cloud density in which these conditions constrain a shaded zone where star formation is allowed. The diagrams are also tested with fully 3-D MHD radiative cooling simulations involving a SNR and a self-gravitating cloud and we find that the numerical analysis is consistent with the results predicted by the diagrams. While the inclusion of a homogeneous magnetic field approximately perpendicular to the impact velocity of the SNR with an intensity ~1 $mu$G results only a small shrinking of the star formation zone in the diagrams, a larger magnetic field (~10 $μ$G) causes a significant shrinking, as expected. Applications of our results to real star formation regions in our own galaxy have revealed that their formation could have been triggered by a SN shock wave. Finally, we have evaluated the effective global star formation efficiency of this sort of interactions and found that it is smaller than the observed values in our Galaxy (SFE ~0.01-0.3). This result is consistent with previous work in the literature and also suggests that the mechanism presently investigated, though very powerful to drive structure formation, supersonic turbulence and eventually, local star formation, does not seem to be sufficient to drive global star formation in normal star forming galaxies.
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