The effect of viscosity and anisotropy in the pressure on the azimuthal motion of the solar wind
The effect of viscosity and anisotropy in the pressure on the azimuthal motion of the solar wind
复制标题
压力中的粘度和各向异性对太阳风方位角运动的影响
DOI：
10.1029/ja075i013p02419
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发表时间：
1970
影响因子：
--
通讯作者：
L. Davis
中科院分区：
文献类型：
--
作者：
E. J. Weber;L. Davis
建立了一个定常轴对称的赤道面附近太阳风流动模型。径向运动被认为是已知的，并研究了方位运动，考虑了磁力、粘度(由磁场修正)和各向异性压力。我们证明，为了得到光滑连续的解，积分常数必须确定，而不是从太阳的边界条件，而是由解在临界半径Ra附近的行为来确定，其中径向马赫数是单位的。粘性显著地增加了5个太阳半径到1个天文单位之间区域的自转倾向。在可被认为是典型条件(温度为2×05°K，径向风速为400公里/秒)的情况下，在地球附近预测的方位向速度约为6公里/秒，而对于非粘性各向同性模式，预测的速度为1公里/秒。
A steady state axially symmetrical model for the flow of the solar wind near the equatorial plane is developed. The radial motion is regarded as known, and the azimuthal motion is investigated, allowing for magnetic forces, viscosity (as modified by the magnetic field), and anisotropic pressure. We show that to obtain a smooth continuous solution the constant of integration has to be determined, not from a boundary condition at the sun, but by the behavior of the solution near the critical radius rA, where the radial Mach number is unity. The viscosity considerably increases the tendency toward corotation in the region between five solar radii and 1 AU. The azimuthal velocity predicted near the earth is of the order of 6 km/sec for what may be regarded as typical conditions (temperature of 2× 05 °K and a radial wind velocity of 400 km/sec), whereas the velocity is 1 km/sec for a nonviscous isotropic model.