The Orion Protostellar Explosion and Runaway Stars Revisited: Stellar Masses, Disk Retention, and an Outflow from the Becklin–Neugebauer Object
The Orion Protostellar Explosion and Runaway Stars Revisited: Stellar Masses, Disk Retention, and an Outflow from the Becklin–Neugebauer Object
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DOI：
10.3847/1538-4357/ab65f2
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发表时间：
2020-01
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影响因子：
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通讯作者：
J. Bally;A. Ginsburg;J. Forbrich;J. Vargas-González
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作者：
J. Bally;A. Ginsburg;J. Forbrich;J. Vargas-González
从猎户座的OMC 1云核喷射出的三颗恒星的自行与它们的质量中心与OMC 1引力束缚的要求相结合，表明射电源I（Src I）可能具有与最近测量一致的约15 M的质量。Src I是自行最小的星星，被怀疑是一颗天文单位尺度的双星，或者是2550年前由动力相互作用产生的原恒星合并残留物。2.2 μm的近红外图像跨越了2021年，证实了“源x”（Src x）的运动距离恒星喷射点和OMC 1原恒星爆炸流出的起源点为2055 km s−1。贝克林-纽介堡（BN）天体和Src I的径向速度和质量限制Src x的径向速度为km s−1。BN附近的几个高自行射电源，包括Zapata 11（[ZRK 2004] 11）和IRc 23附近的一个扩散源，可能追踪到BN的缓慢双极流出。Src I周围的巨大圆盘可能是在恒星抛射之前存在的圆盘的幸存部分。虽然受到N体相互作用的高度扰动、冲击和重定向，但已经有足够的时间让圆盘松弛，其自旋轴大致垂直于自行。
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 M⊙ consistent with recent measurements. Src I, the star with the smallest proper motion, is suspected to be either an astronomical-unit-scale binary or a protostellar merger remnant produced by a dynamic interaction ∼550 yr ago. Near-infrared 2.2 μm images spanning ∼21 yr confirm the ∼55 km s−1 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 km s−1. 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 reoriented 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.