The 3-D plasma distribution function analyzers with time-of-flight mass discrimination for Cluster, FAST, and Equator-S
The 3-D plasma distribution function analyzers with time-of-flight mass discrimination for Cluster, FAST, and Equator-S
复制标题
具有飞行时间质量辨别功能的 3-D 等离子体分布函数分析仪，适用于 Cluster、FAST 和 Equator-S
DOI：
10.1029/gm102p0243
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发表时间：
2013
期刊：
影响因子：
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通讯作者：
M. Steinacher
中科院分区：
文献类型：
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作者：
E. Möbius;L. Kistler;M. Popecki;K. Crocker;M. Granoff;Y. Jiang;E. Sartori;V. Ye;H. Rème;J. Sauvaud;A. Cros;C. Aoustin;T. Camus;J. Médale;J. Rouzaud;C. Carlson;J. Mcfadden;D. Curtis;H. Heetderks;J. Croyle;C. Ingraham;B. Klecker;D. Hovestadt;M. Ertl;F. Eberl;H. Kästle;E. Kunneth;P. Laeverenz;E. Seidenschwang;E. Shelley;D. Klumpar;E. Hertzberg;G. Parks;M. McCarthy;A. Korth;H. Rosenbauer;B. Gräve;L. Eliasson;S. Olsen;H. Balsiger;U. Schwab;M. Steinacher
一个类似的飞行时间等离子体分析仪系统将作为CODIF（成分和扩散函数分析仪）在四个星团航天器上飞行，作为ESIC（赤道-S离子成分仪）在赤道-S上飞行，作为TEAMS（飞行时间能角质谱仪）在FAST上飞行。这些仪器将首次允许在1/2或1个自旋周期内确定单个离子种类的三维分布函数。这对于研究磁层不同区域的选择性磁层过程至关重要。该传感器由一个环形的顶帽静电分析器组成，其瞬时接受的离子的极角超过360°。对于星团和赤道-S，这个范围被细分为两半，几何因子相差100倍，以科普磁层中通量的宽动态范围。对于FAST，时间分辨率增加了两倍，以便通过同时使用两个半部分来关注快速极光现象。在将入射离子后加速至25 kV后，飞行时间质谱仪可区分各个种类。校准运行表明，该仪器能很容易地分离出H +、He 2+、He +、O +和3 ~ 20 keV后加速的能量，甚至能分离出O 2 +分子。板上的歧视，积累和时刻计算允许有效的检索数据流。
A similar time-of-flight plasma analyzer system will be flown as CODIF (COmposition and Dlstribution Function analyzer) on the four Cluster spacecraft, as ESIC (Equator-S Ion Composition instrument) on Equator-S, and as TEAMS (Time-of-flight Energy Angle Mass Spectrograph) on FAST. These instruments will for the first time allow the 3-dimensional distribution functions of individual ion species to be determined within 1/2 or 1 spin period. This will be crucial for the study of selective energization processes in various regions of the magnetosphere. The sensor consists of a toroidal top-hat electrostatic analyzer with instantaneous acceptance of ions over 360° in polar angle. For Cluster and Equator-S this range is subdivided into two halves with geometric factors different by a factor of 100 in order to cope with the wide dynamic range of fluxes in the magnetosphere. For FAST the time resolution is increased by a factor of two to focus on fast auroral phenomena by using both halves simultaneously. After post-acceleration of the incoming ions by up to 25 kV, a time-of-flight mass spectrograph discriminates the individual species. It has been demonstrated in calibration runs that the instruments can easily separate H + , He 2+ , He + , O + and for energies after post-acceleration of 3 20 keV even O 2 + molecules. On board discrimination, accumulation, and moment computation allow efficient retrieval of the data stream.