Rotational Evolution of Solar-Type Stars. I. Main-Sequence Evolution
Rotational Evolution of Solar-Type Stars. I. Main-Sequence Evolution
复制标题
太阳型恒星的旋转演化。
DOI：
10.1086/170269
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发表时间：
1991
期刊：
影响因子：
--
通讯作者：
M. Brenner
中科院分区：
文献类型：
--
作者：
K. Macgregor;M. Brenner
提出了一个简单的参数化模型，用于太阳型恒星内部角动量的重新分布。通过将其与磁耦合风作用引起的角动量损失的描述相结合，可以追踪低质量矮星在各种初始条件和参数规格下的旋转历史。讨论了 1 个太阳质量恒星的旋转演化的计算结果，从它到达零年龄主序带的时间到当今太阳的年龄。最好的一致性是与以下观测约束条件一致：(1) 表面磁场强度在很大程度上独立于快速旋转的表面角速度 omega，并且近似线性地依赖于近似太阳值的 omega；(2) 从核心到对流区的角动量转移的时间尺度，在整个演化过程中基本保持恒定，其大小约为 1000 万年。该值约等于初始风制动时间。这些结果是在太阳型恒星辐射内部磁场对角动量重新分布的定性描述的背景下讨论的。 48 参考文献
A simple, parameterized model for the redistribution of angular momentum within the interiors of solar-type stars is presented. By incorporating it with a description of angular momentum loss through the action of a magnetically coupled wind, tracing the rotational histories of low-mass dwarf stars for a variety of initial conditions and parameter specifications is accomplished. The results of calculations are discussed for the rotational evolution of a 1 solar mass star, from the time of its arrival on the zero-age main sequence to the age of the present-day sun. Best agreement is with observational constraints for (1) a surface magnetic field strength which is largely independent of surface angular velocity omega for rapid rotation, and approximately linearly dependent on omega for approximately solar values, and (2), a time scale for angular momentum transfer from the core to the convection zone which remains essentially constant throughout the evolution, with magnitude of a about 10 million yr. This value is approximately equal to the initial wind braking time. These results are discussed in the context of a qualitative description of angluar momentum redistribution by magnetic fields in the radiative interiors of solar-type stars. 48 refs.