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首页> 外文会议>7th Spacecraft Charging Technology Conference 2001: a Spacecraft Charging Odyssey, Apr 23-27, 2001, Noordwijk, the Netherlands >THE PLASMA ENVIRONMENT AROUND MERCURY
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THE PLASMA ENVIRONMENT AROUND MERCURY

机译：汞周围的等离子体环境

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摘要

Our understanding of the plasma environment of planet Mercury is mostly derived from the limited amount of data which has been collected by the NASA flyby mission, Mariner 10, in 1974-1975. The prospect for new missions, the NASA Messenger orbiter and the ESA BepiColombo cornerstone have, however, stimulated a renewed interest in this planet. Like the Moon, Mercury has a vestigial atmosphere and no ionosphere, but - against all expectations - it possesses a small, but definite, intrinsic magnetic field. Due to the weakness of this field, of the order of a few 100 nT at the equator, and the relatively high solar wind pressure which prevails at the orbit of Mercury, the size of the magnetospheric cavity is much smaller than that of the Earth. The two environments have somewhat similar topologies but their dynamics differ widely. The solar wind may even reach the surface of Mercury when its pressure is sufficiently large. The formation of radiation belts is probably impeded for lack of a sufficiently strong magnetic confinement. The environment is permeated by a current system which is basically unknown and the plasma is rarefied, like in the Earth magnetosphere. Due to the proximity of the Sun, the emission rate of photoelectrons is up to 10 times larger than at the Earth orbit and leads to unique electrostatic phenomena oh orbiting spacecraft and at the surface of the planet.
机译：我们对水星行星等离子环境的了解主要来自1974-1975年NASA飞行任务水手10号所收集的有限数据。然而，新任务的前景，NASA信使轨道器和ESA BepiColombo基石激发了人们对该星球的新兴趣。像月球一样，水星具有残留的气氛，没有电离层，但是-出乎所有人的意料-它拥有一个很小但确定的固有磁场。由于磁场的弱点，在赤道处约为100 nT的量级，并且在水星轨道上普遍存在着相对较高的太阳风压，因此磁层空腔的大小比地球小得多。两种环境的拓扑结构有些相似，但是它们的动态差异很大。当太阳风的压力足够大时，它甚至可能到达汞的表面。辐射带的形成可能由于缺乏足够强的磁性限制而受到阻碍。像地球磁层一样，环境被目前未知的电流系统所渗透，并且等离子体被稀化了。由于太阳的接近，光电子的发射速率是地球轨道的10倍之多，并导致在航天器和行星表面发生独特的静电现象。

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