论文标题
猎户座原始爆炸和失控的星星重新审视：恒星群体，磁盘保留和BN的流出
The Orion Protostellar Explosion and Runaway Stars Revisited: Stellar Masses, Disk Retention, and an Outflow from BN
论文作者
论文摘要
从Orion的Omc1云芯弹出的三颗恒星的适当运动与其质量中心在重力上与OMC1结合的要求结合在一起，以表明无线电源I（SRC I）可能在15个太阳能质量上可能与最近的测量相一致。 SRC I（具有最小的适当运动的恒星）被怀疑是Au级二元的二进制或原动性合并残余，该二进制是由〜550年前的动态相互作用产生的。近21年的近红外2.2 UM图像确认了距离恒星射血点的位置和爆炸性OMC1 Protostellar流出的原点的〜55 km/s运动。 Becklin-Neugebauer（BN）对象和SRC I的径向速度和质量将SRC X的径向速度限制为V_ {LSR} = -28 +/- 10 km/s。 BN附近的几个高度运动无线电源，包括Zapata 11（[ZRK2004] 11）和IRC 23附近的漫射源，可能会追踪BN的慢速双极流出。 SRC I周围的巨大磁盘可能是恒星弹出之前存在的磁盘的存活部分。尽管高度扰动，震惊和重新定向了N体相互作用，但已经经过了足够的时间，以使磁盘用旋转轴大致正交与适当的运动放松。
The proper motions of the three stars ejected from Orion's OMC1 cloud core are combined with the requirement that their center of mass is gravitationally bound to OMC1 to show that radio source I (Src I) is likely to have a mass around 15 Solar masses consistent with recent measurements. Src I, the star with the smallest proper motion, is suspected to be either an AU-scale binary or a protostellar merger remnant produced by a dynamic interaction ~550 years ago. Near-infrared 2.2 um images spanning ~21 years confirm the ~55 km/s motion of `source x' (Src x) away from the site of stellar ejection and point of origin of the explosive OMC1 protostellar outflow. The radial velocities and masses of the Becklin-Neugebauer (BN) object and Src I constrain the radial velocity of Src x to be V_{LSR} = -28 +/-10 km/s . Several high proper-motion radio sources near BN, including Zapata 11 ([ZRK2004] 11) and a diffuse source near IRc 23, may trace a slow bipolar outflow from BN. The massive disk around Src I is likely the surviving portion of a disk that existed prior to the stellar ejection. Though highly perturbed, shocked, and re-oriented by the N-body interaction, enough time has elapsed to allow the disk to relax with its spin axis roughly orthogonal to the proper motion.
