A radiation-driven disc wind model for massive young stellar objects
A radiation-driven disc wind model for massive young stellar objects
复制标题
大质量年轻恒星体的辐射驱动盘风模型
DOI：
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复制
发表时间：
1998
期刊：
影响因子：
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通讯作者：
J. Stone
中科院分区：
文献类型：
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作者：
J. Drew;D. Proga;J. Stone
辐射驱动的盘风模型的建议，提供了很大的希望，解释极端的质量损失签名的大规模年轻恒星的对象（BN型对象和更明亮的赫比格Be星）。有人认为，与年轻的晚O/早B星相关的密集低速风是持续光学厚吸积的结果。从开普勒盘流出的气流允许风速为200 km s 1，这大大低于从恒星表面逃逸的速度。星星本身不需要快速旋转。在流体动力学计算中考虑了圆盘辐照，并从观测和动力学角度确定了圆盘辐照是一个重要的问题。
A radiation-driven disk wind model is proposed that offers great promise of explaining the extreme mass loss signatures of massive young stellar objects (the BN-type objects and more luminous Herbig Be stars). It is argued that the dense low-velocity winds associated with young late-O/early-B stars would be the consequence of continuing optically-thick accretion onto them. The launch of outflow from a Keplerian disk allows wind speeds of �200 km s 1 that are substantially less than the escape speed from the stellar surface. The star itself is not required to be a rapid rotator. Disk irradiation is taken into account in the hydrodynamical calculation presented, and identified as an important issue both observationally and from the dynamical point of view.