We analyse two high-resolution 2D hybrid simulations of plasma turbulence with observation-driven initial conditions that are representative of the near-Sun and the near-Earth solar wind. The former employs values of some fundamental parameters that have been measured by the Parker Solar Probe at 0.17 au from the Sun, while, in the latter, they are set to average values typically observed at 1 au. We compare the spatial and spectral properties of the magnetic, ion velocity, and density fluctuations, as well as the time evolution of magnetic reconnection events that occur spontaneously as the result of the development of turbulence. Despite some differences due to the different plasma conditions, some key features are observed in both simulations: elongated ion-scale Alfvénic structures form in between vortices whenever the orientation of the magnetic field lines is the same, i.e., magnetic reconnection via the formation of an X point cannot occur; the magnetic and density fluctuations at sub-ion scales are governed by force balance; the magnetic compressibility at sub-ion scales is compatible with isotropic magnetic field components; the characteristic time of the formation of current sheets is the eddy turnover at the energy injection scale, while the characteristic time for their disruption via reconnection is compatible with the Alfvén time of the background turbulence.

中文翻译：

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近太阳风和近地太阳风中的等离子体湍流：通过观测驱动的二维混合模拟进行的比较

我们分析了等离子体湍流的两个高分辨率二维混合模拟，这些模拟具有代表近太阳和近地太阳风的观测驱动初始条件。前者采用帕克太阳探测器在距太阳 0.17 au 处测量的一些基本参数的值，而在后者中，它们设置为通常在 1 au 处观察到的平均值。我们比较了磁、离子速度和密度波动的空间和光谱特性，以及由于湍流发展而自发发生的磁重联事件的时间演化。尽管由于不同的等离子体条件存在一些差异，但在两种模拟中都观察到了一些关键特征：只要磁场线的方向相同，即不会发生通过形成 X 点的磁重联，就会在涡旋之间形成细长的离子尺度 Alfvénic 结构；亚离子尺度的磁和密度波动受力平衡控制；亚离子尺度的磁可压缩性与各向同性磁场分量兼容；电流片形成的特征时间是能量注入尺度下的涡流转换，而它们通过重新连接破坏的特征时间与背景湍流的 Alfvén 时间兼容。亚离子尺度的磁可压缩性与各向同性磁场分量兼容；电流片形成的特征时间是能量注入尺度下的涡流转换，而它们通过重新连接破坏的特征时间与背景湍流的 Alfvén 时间兼容。亚离子尺度的磁可压缩性与各向同性磁场分量兼容；电流片形成的特征时间是能量注入尺度下的涡流转换，而它们通过重新连接破坏的特征时间与背景湍流的 Alfvén 时间兼容。