Recent reports of the first data from Parker Solar Probe (PSP) have pointed to a series of links, correlations or anti-correlations between the solar wind bulk speed ( $V_{\mathrm{SW}}$ ) and physical properties of plasma particles from less than 0.25 AU in the corona. In the present paper, we describe corresponding and additional links of solar wind properties, at 0.4 AU and 1.0 AU, in an attempt to complement the PSP data and understand their evolution. A detailed analysis is carried out for the main electron populations, comparing the low-energy (thermal) core and the collisionless suprathermal halo. We show that the anti-correlation observed at 0.4 AU between $V_{\mathrm{SW}}$ and the number density (average value) is maintained also at 1 AU for both the core and halo electrons. On the contrary, only the core electrons manifest a clear anti-correlation of the temperature with $V_{\mathrm{SW}}$ , while the halo temperature does not vary much. We also describe the ions, protons and helium, which have a more reduced mobility and their properties exhibit different variations with the solar wind speed. The results are used to shed more light on the mechanisms leading to a differential acceleration of these species and the origin of slow and fast wind modulation.

中文翻译：

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由流速组织的太阳风等离子体粒子

帕克太阳探测器 (PSP) 的第一批数据的最新报告指出了太阳风体积速度 ($V_{\mathrm{SW}}$) 与等离子体粒子物理特性之间的一系列联系、相关性或反相关性来自日冕中小于 0.25 AU。在本文中，我们描述了 0.4 AU 和 1.0 AU 太阳风属性的相应和附加链接，以尝试补充 PSP 数据并了解它们的演变。对主要电子群进行了详细分析，比较了低能（热）核心和无碰撞超热晕。我们表明，在 $V_{\mathrm{SW}}$ 和数密度（平均值）之间在 0.4 AU 处观察到的反相关性对于核心和晕电子也保持在 1 AU。相反，只有核心电子表现出明显的温度与 $V_{\mathrm{SW}}$ 的反相关，而光晕温度变化不大。我们还描述了离子、质子和氦，它们的迁移率更低，并且它们的特性随着太阳风速表现出不同的变化。这些结果用于更多地阐明导致这些物种差异加速的机制以及慢速和快速风调制的起源。