Angular Momentum Transport in the Sun’s Radiative Zone by Gravito-Inertial Waves
Angular Momentum Transport in the Sun’s Radiative Zone by Gravito-Inertial Waves
复制标题
引力惯性波在太阳辐射区的角动量传输
DOI：
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发表时间：
2008
期刊：
影响因子：
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通讯作者：
J. Zahn
中科院分区：
文献类型：
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作者：
S. Mathis;S. Talon;Florian Pantillon;J. Zahn
重力内波是角动量远距离传输的有效过程。它们现在被认为是理解恒星自转演化的重要组成部分，可以解释太阳的准平坦内部自转轮廓。由于太阳的自转频率与波的自转频率在同一量级，现在有必要改进我们对波传播的描述，并以相干的方式考虑科里奥利加速度的作用。为了实现这一目标，我们采用传统的近似，它可以适用于恒星辐射区的条件下，给。我们提出了修改后的输运方程和它们的数值评估的参数范围内，这是显着的太阳。讨论了角动量在太阳辐射区和恒星辐射区内传输的结果。
Internal gravity waves constitute an efficient process for angular momentum transport over large distances. They are now seen as an important ingredient in understanding the evolution of stellar rotation and can explain the Sun’s quasi-flat internal-rotation profile. Because the Sun’s rotation frequency is of the same order as that of the waves, it is now necessary to refine our description of wave propagation and to take into account the action of the Coriolis acceleration in a coherent way. To achieve this goal, we adopt the traditional approximation, which can be applied to stellar radiation zones under conditions that are given. We present the modified transport equations and their numerical evaluation in a parameter range that is significant for the Sun. Consequences for the transport of angular momentum inside solar and stellar radiative regions are discussed.