金星弓激波与离子成分边界位置的驱动因素排名
Ranking the drivers of the Venusian bow shock and ion composition boundary locations
AI总结：
本文结合多种统计方法，分析排名金星弓激波与离子成分边界的驱动因素，明确两类边界的主要驱动因子，对比火星与金星的相关结果并分析极端偏移的驱动因素。
AI中文摘要：
金星与太阳风的相互作用会形成由等离子体边界构成的感应磁层，其动力学过程因外部（太阳光子、太阳风等离子体、行星际磁场IMF）和内部（电离大气）驱动因素的共同影响而十分复杂。研究这些驱动因素有助于理解能量与动量在金星系统内的传递，进而为通过与太阳风耦合的大气侵蚀过程研究提供支撑。本文基于金星快车的观测数据，结合赤池信息准则、最小绝对收缩选择算子回归、偏相关分析等多种方法，对金星弓激波与离子成分边界位置的主要驱动因素的影响进行分析与排名，同时重新审视了Signoles等人（2023）的研究结果。这些方法可用于识别可能干扰解释的交叉相关性，并通过稳健方法对驱动因素进行排名。研究发现，弓激波主要由IMF强度或马赫数、区分准垂直与准平行激波的IMF θbn角驱动，其次是太阳极紫外通量和太阳动压（对流电场诱导的不对称性影响较小）；离子成分边界主要由极紫外通量驱动，太阳风参数和IMF诱导的磁堆积不对称性影响较弱。本文还对比了两种边界的行为，以及火星与金星弓激波的驱动因素排名，最后对极端弓激波和离子成分边界偏移的驱动因素进行了分析。
英文摘要：
The Venusian interaction with the solar wind leads to the formation of an induced magnetosphere structured by plasma boundaries. Their dynamics is complex, due to the combined influence of external (solar photons, solar wind plasma and interplanetary magnetic field (IMF)) and internal (ionized atmosphere) drivers. Studying these drivers helps understanding the transfer of energy and momentum throughout the Venusian system, and has thus implications for the erosion of the atmosphere through its coupling with the solar wind. We here analyze and rank the influence of the main drivers of the Venusian bow shock and ion composition boundary locations. We revisit the results by Signoles et al. (2023) based on Venus Express measurements by combining several methods such as the Akaike Information Criterion, Least Absolute Shrinkage Selection Operator regression, and partial correlations. These methods allow to investigate cross correlations that appear and can bias the interpretation, and allow to rank drivers with robust approaches. The bow shock appears primarily driven by the IMF intensity or Mach number, the IMF $θ_{bn}$ angle separating quasi-perpendicular vs quasi-parallel shocks, and then the solar extreme ultraviolet fluxes and solar wind dynamic pressure (with little influence of the convective electric field induced asymmetries). The Ion Composition Boundary is primarily driven by extreme ultraviolet fluxes, with a more reduced influence of several solar wind parameters and IMF induced magnetic pileup asymmetries. We also compare the behaviors of both boundaries and then compare the bow shock driver rankings at Mars and Venus. Finally we propose an analysis of the drivers of the extreme bow shock and ion composition boundary excursions.
