火星感应磁层边界观测研究进展  

Review of observations on the boundary of the Martian induced magnetosphere

作　　者：王晶 Wang Jing(Planetary Environmental and Astrobiological Research Laboratory(PEARL),School of Atmospheric Sciences,Sun Yat-sen University,Zhuhai 519082,China)

机构地区：[1]中山大学大气科学学院空间与行星科学系,珠海519082

出　　处：《地球与行星物理论评(中英文)》2025年第4期421-445,共25页Reviews of Geophysics and Planetary Physics

基　　金：国家自然科学基金资助项目(42261160643);国家自然科学基金青年基金资助项目(42304174);广东省基础与应用基础研究基金资助项目(2024A1515011495,2021A1515110315)。

摘　　要：关于太阳风-火星相互作用边界的探测研究几乎贯穿了整个火星空间探测的历史.太阳风-火星相互作用区中间总是存在一个边界,即火星感应磁层边界.过去几十年,受火星探测器所携带仪器种类和精度的限制,火星感应磁层边界一直基于单一或部分仪器探测数据来定义,导致其具有多种多样的名称,如,离子成分边界、感应磁层边界、磁堆积边界等.本文沿着Phobos-2、MGS、MEX以及MAVEN等一系列火星探测器的探测历程,简单梳理了火星感应磁层边界观测研究的发展.总结了具有不同名称的边界的物理特征和定义标准及其之间的位置关系.最新研究基于MAVEN探测器的等离子体和磁场综合探测数据,研究证实了火星感应磁层边界为磁流体动力学间断面,其物理性质与地球磁层顶类似.磁场的堆积位于边界间断面的上游,其性质更类似于地球磁层顶上游的等离子体耗尽层.相关工作进一步厘清了太阳风-火星相互作用边界的结构和物理性质.最早对太阳风-火星相互作用边界的认识来自于Phobos-2探测器对火星等离子体边界的报道.太阳风等离子体流在火星电离层上方几百公里处停滞,形成阻碍太阳风的边界,当时被称为质子边界.在该边界附近,同样观测到了将上游太阳风质子和下游行星氧离子分隔开的边界,称为离子成分边界.同时,还观测到了穿出边界时强电场波动消失的特征,称作行星顶.这三种边界可能重合.由于当时对火星磁场研究的不足,还无法确定该边界是否由行星内禀磁场的障碍产生.随着MEX和MAVEN探测器提供了对等离子体观测的更精确数据,离子成分边界有了更清晰的定义,即边界将其上下游分别由太阳风质子和火星重离子(如O^(+)和O_(2)^(+))主导的等离子体分隔开来,上游的太阳风质子流在边界处停滞.Phobos-2探测器上携带的电磁场仪器,在太阳风-火星相互作用区探测到�The boundary of the Mars-solar wind interaction has been investigated throughout the history of Mars space exploration.There is always a boundary between the solar wind and Mars,namely the boundary of the Martian induced magnetosphere.In the past few decades,due to the limitations of the types and accuracy of instruments on board Mars probes,the definition of the boundary of the Martian induced magnetosphere has been based on single or partial instrument data,resulting in different boundary names,such as the ion composition boundary,the induced magnetosphere boundary,and the magnetic pile-up boundary.This article briefly reviews the development of the observational studies on the boundary of the Martian induced magnetosphere along the exploration history of a series of Mars probes such as Phobos-2,MGS,MEX,and MAVEN,and summarizes the physical characteristics and definition criteria of boundaries with different names,as well as their positional relationships.Based on the comprehensive detection data of plasma and magnetic field from MAVEN,it is confirmed that the boundary of the Martian induced magnetosphere is a magnetohydrodynamic discontinuity,and its physical properties are similar to those of the Earth's magnetopause.The pile-up process of the magnetic fields occurs upstream of the discontinuity,and its properties resemble those of the plasma depletion layer upstream of the Earth's magnetopause.The relevant work clarified the structure and physical properties of the Mars-solar wind interaction boundary.The earliest knowledge of the Mars-solar wind interaction boundary came from the reporting on the plasma boundary by Phobos-2.The solar wind flow was blocked several hundred kilometers above the Martian ionosphere,forming a boundary known as the protonopause.Near the protonopause,another boundary termed the ion composition boundary(ICB),was observed that separates upstream solar wind protons from downstream planetary oxygen ions.Meanwhile,a boundary,referred to as the planetpause,characterized by the disappeara

关 键 词：太阳风-火星相互作用边界 火星感应磁层边界 火星磁堆积边界 火星离子成分边界 火星感应磁层顶 

分 类 号：P351[天文地球—空间物理学]