A Rotating, Magnetic, Radiation-driven Wind Model for Wolf-Rayet Stars
A Rotating, Magnetic, Radiation-driven Wind Model for Wolf-Rayet Stars
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沃尔夫拉叶星旋转、磁性、辐射驱动的风模型
DOI：
10.1086/167159
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发表时间：
1989
期刊：
影响因子：
--
通讯作者：
J. Cassinelli
中科院分区：
文献类型：
--
作者：
C. H. Poe;D. B. Friend;J. Cassinelli
为了解决风动量问题，对WR星应用了一个包含旋转和开放磁场影响的辐射驱动风模型。对于赤道区域的流动，研究了质量损失率和末端速度与旋转速度和表面磁场的关系。在恒星光度符合Maeder质量光度关系的情况下，研究了从纯辐射驱动风到旋转磁驱动风的转变。WR风的另一种图像是，在高纬度有较慢但较密集的赤道气流和较快的辐射驱动风。给出了几个恒星的风模型，它们与内部理论是一致的。如果恒星的磁场约为1500G，并且自转速度大于最大值的85%，它们就可以满足射电和紫外线观测，解释动量问题，并克服自旋问题。参考文献52篇。
A radiation-driven wind model that incorporates the effects of rotation and an open magnetic field is applied to WR stars in order to address the wind momentum problem. The dependence of the mass-loss rate and terminal velocity on the rotation rate and surface magnetic field is studied for the flow in the equatorial region. The transition from a purely radiatively driven wind to a rotationally and magnetically driven wind is investigated for the case in which the stellar luminosity is consistent with Maeder's mass-luminosity relation. An alternative picture for WR winds is developed in which there is a slower but denser equatorial flow and a fast radiation-driven wind at higher latitudes. Wind models for several stars are presented that are consistent with interior theory. If the stars have field of about 1500 G and rotate at rates greater than about 85 percent maximum, they can satisfy the radio and UV observations and explain the momentum problem, and also overcome the spindown problem. 52 references.