Turbulence, a ubiquitous phenomenon in interplanetary space, is crucial for the energy conversion of space plasma at multiple scales. This work focuses on the propagation, polarization, and wave composition properties of the solar wind turbulence within 0.3 au, and its variation with heliocentric distance at magnetohydrodynamic scales (from 10 s to 1000 s in the spacecraft frame). We present the probability density function of propagation wavevectors (PDF ( k ∥ , k ⊥ )) for solar wind turbulence within 0.3 au for the first time: (1) wavevectors cluster quasi-(anti-)parallel to the local background magnetic field for kd i < 0.02, where d i is the ion inertial length; (2) wavevectors shift to quasi-perpendicular directions for kd i > 0.02. Based on our wave composition diagnosis, we find that: the outward/anti-sunward Alfvén mode dominates over the whole range of scales and distances, the ...

中文翻译：

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派克太阳探测器观测到的0.3 au之内的磁流体动力湍流的波组成，传播和极化

湍流是行星际空间中普遍存在的现象，对于空间等离子体在多个尺度上的能量转换至关重要。这项工作的重点是在0.3 au以内的太阳风湍流的传播，极化和波组成特性，以及它在磁流体动力学尺度上（在航天器框架中从10 s到1000 s）随日心距的变化。我们首次提出了在0.3 au以内的太阳风湍流传播波矢量（PDF（k∥，k⊥））的概率密度函数：（1）波矢量集准（反）平行于局部背景磁场kd i <0.02，其中di是离子惯性长度；（2）当kd i> 0.02时，波向量向准垂直方向移动。根据我们的波成分诊断，我们发现：