非WKB Alfven波对具有微分离子流的多分量太阳风的影响
Effects of non-WKB Alfven waves on a multicomponent solar wind with differential ion flow
摘要：
我们提出了多组分太阳风模型自洽地将无耗散，单色，有限波长（非WKB），磁流体，环形Alfvén波的贡献，这是耦合到流只通过有质动力。我们发现，非WKB的影响是显着的，快速和缓慢的太阳风的解决方案一样。与它们的非WKB对应物相比，WKB在加速阿尔芬点内的太阳风方面更有效，产生显着增强的离子通量和显着减少的内日冕中的α丰度。只有当$ω\gtrsim 3.5\times 10^{-3}$（$1.5\times 10^{-3}$）$\rm rad s^{-1}$满足时，快（慢）风模式才能被WKB模式充分近似。此外，虽然阿尔文波一般倾向于减小质子-α速度差$|U_{αp}|$的幅度，但不同的机制在由$ω_c\sim {several}\times 10^{-5}$ $\rm rad s^{-1}$分隔的两个不同的区域中运行。当使用$ω> ω_c$时，波动是波浪状的，并且倾向于加速两种离子物质，从而通过对离子流做功而损失它们的大部分能量;而当使用$ω< ω_c$时，准静态行为产生：该波动可在计算域的大部分中加速较慢流动的离子种类但减速较快移动的离子种类，并且在底部注入的波能通量中只有一小部分损失。讨论了$ω_c$对质子和α粒子速度涨落谱的影响，这些结果可能被未来的太阳轨道飞行器和太阳探测器等探测任务所获得。
英文摘要：
We present multicomponent solar wind models self-consistently incorporating the contribution from dissipationless, monochromatic, finite-wavelength (non-WKB), hydromagnetic, toroidal Alfvén waves, which are coupled to the flow only through the ponderomotive forces. We find that the non-WKB effects are significant, for the fast and slow solar wind solutions alike. Compared with their non-WKB counterparts the WKB ones are more effective in accelerating the solar wind inside the Alfvén point, producing significantly enhanced ion fluxes and considerably reduced alpha abundance in the inner corona. Only when $ω\gtrsim 3.5\times 10^{-3}$ ($1.5\times 10^{-3}$) $\rm rad s^{-1}$ can the fast (slow) wind models be adequately approximated by the WKB one. Moreover, while the Alfvén waves tend to reduce the magnitude of the proton-alpha speed difference $|U_{αp}|$ in general, different mechanisms operate in two different regimes separated by an $ω_c\sim {several}\times 10^{-5}$ $\rm rad s^{-1}$. When $ω> ω_c$, the fluctuations are wave-like and tend to accelerate both ion species, thereby losing most of their energy by doing work on ion flows; whereas when $ω< ω_c$, a quasi-static behavior results: the fluctuations may act to accelerate the slower flowing ion species but decelerate the faster moving one in a large portion of the computational domain, and only a minor fraction of the wave energy flux injected at the base is lost. The consequences of $ω_c$ on the velocity fluctuation spectra of protons and alpha particles, which are likely to be obtained by future missions like Solar Orbiter and Solar Probe, are discussed.
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