论文标题
恒星形成区域IC 1396N中原恒星喷气机的碰撞。打结的分析适当动作
Collision of protostellar jets in the star-forming region IC 1396N. Analysis of knot proper motions
论文作者
论文摘要
据信，明亮的云IC 1396N拥有少数已知的案例之一，其中两个双极共同流出了由年轻的恒星物体驱动的实际上碰撞。 CO流出通过H_2发射的结链来追溯，并在可能的碰撞位置提高发射。 这项工作的目的是使用H_2节的适当动作来确认碰撞方案。 获得了第二个时期的H_2图像，并以〜11年的时间基线确定结的适当运动。我们还对图像进行了微分光度法，以检查结的通量变化。 对于每个流出（N和S），我们将结归类为前碰撞或后碰撞。估计了前碰撞结的轴，可能的碰撞点的位置以及后结节结的轴。还计算了碰撞后结的适当运动方向与碰撞点的位置角之间的差异。对于某些结，我们使用源自H_2光谱的径向速度获得了3D速度。 相互作用区域中H_2结的速度模式（碰撞后结）显示出与前结节的偏差，这与两种流出之间相互作用的结果一致。这有利于对IC 1396N的解释流出为两种原始喷气机之间的真实碰撞，而不是投影效应。
The bright-rimmed cloud IC 1396N is believed to host one of the few known cases where two bipolar CO outflows driven by young stellar objects actually collide. The CO outflows are traced by chains of knots of H_2 emission, with enhanced emission at the position of the possible collision. The aim of this work is to use the proper motions of the H_2 knots to confirm the collision scenario. A second epoch H_2 image was obtained, and the proper motions of the knots were determined with a time baseline of ~11 years. We also performed differential photometry on the images to check the flux variability of the knots. For each outflow (N and S) we classified the knots as pre-collision or post-collision. The axes of the pre-collision knots, the position of the possible collision point, and the axes of the post-collision knots were estimated. The difference between the proper motion direction of the post-collision knots and the position angle from the collision point was also calculated. For some of the knots we obtained the 3D velocity by using the radial velocity derived from H_2 spectra. The velocity pattern of the H_2 knots in the area of interaction (post-collision knots) shows a deviation from that of the pre-collision knots, consistent with being a consequence of the interaction between the two outflows. This favours the interpretation of the IC 1396N outflows as a true collision between two protostellar jets instead of a projection effect.
