具有不同流动的热各向异性离子的多组分太阳风中的Angular momentum传输
Angular momentum transport in a multicomponent solar wind with differentially flowing, thermally anisotropic ions
摘要：
Helios对快速太阳风的角动量通量$L$的测量表明，单个离子的贡献，$L_p$和$L_α$，往往是负的（即，与太阳反向旋转）。然而，对于慢风，情况正好相反，总粒子贡献$L_P = L_p + L_α$趋于超过磁贡献$L_M$。这些方面与以前的模型不同。我们研究是否引入现实的离子温度各向异性可以解决这个矛盾。从一般的多流体输运方程与gyrotropic物种的压力张量，我们推导出方程的一般轴对称，旋转的恒星风，包括两个主要的离子物种的dupronal和方位角动力学。方位角动力学进行了详细的研究，使用经验构造的纬向流剖面的太阳风。我们发现$L$是由要求总角动量守恒定律的解是唯一的和光滑的阿尔芬点，其中组合阿尔芬马赫数$M_T=1$。与各向同性情况相比，引入现实离子温度各向异性可引入高达10%的$L$变化和高达1.8 km/s的0.3和1 AU之间的单个离子的方位角速度变化。后者对$L_P$和$L_M$的相对重要性有很大影响。然而，引入离子温度各向异性不能解决测量和模型之间的差异。对于快风解，虽然在极端情况下$L_P$变为负值，但$L_p$永远不会变为负值。另一方面，对于慢风解，$L_P$永远不会超过$L_M$，即使$L_M$可能小于单个离子的贡献，因为$L_p$和$L_α$对于慢风和快风总是具有相反的符号。
英文摘要：
The Helios measurements of the angular momentum flux $L$ for the fast solar wind show that the individual ion contributions, $L_p$ and $L_α$, tend to be negative (i.e., in the sense of counter-rotation with the Sun). However, the opposite holds for the slow wind, and the overall particle contribution $L_P = L_p + L_α$ tends to exceed the magnetic one $L_M$. These aspects are at variance with previous models. We examine whether introducing realistic ion temperature anisotropies can resolve this discrepancy. From the general multifluid transport equations with gyrotropic species pressure tensors, we derive the equations governing both the meridional and azimuthal dynamics of general axisymmetrical, rotating stellar winds that include two major ion species. The azimuthal dynamics are examined in detail, using the empirically constructed meridional flow profiles for the solar wind. We find that $L$ is determined by requiring that the solution to the total angular momentum conservation law is unique and smooth close to the Alfven point, where the combined Alfvenic Mach number $M_T=1$. Introducing realistic ion temperature anisotropies may introduce a change of up to 10% in $L$ and up to 1.8 km/s in azimuthal speeds of individual ions between 0.3 and 1 AU, compared with the isotropic case. The latter has strong consequences on the relative importance of $L_P$ and $L_M$. However, introducing ion temperature anisotropies cannot resolve the discrepancy between measurements and models. For the fast-wind solutions, while in extreme cases $L_P$ becomes negative, $L_p$ never does. On the other hand, for the slow-wind solutions, $L_P$ never exceeds $L_M$, even though $L_M$ may be less than the individual ion contribution, since $L_p$ and $L_α$ always have opposite signs for the slow and fast wind alike.
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