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首页> 外文会议>Cluster and double star symposium >FIVE YEARS OF INVESTIGATION OFWHISTLER-MODE CHORUS USING THEMEASUREMENTS OF THE CLUSTER SPACEFLEET
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FIVE YEARS OF INVESTIGATION OFWHISTLER-MODE CHORUS USING THEMEASUREMENTS OF THE CLUSTER SPACEFLEET

机译：利用集群空间的方法对惠斯勒模式合唱团进行调查的五年

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We summarize results obtained during investigation ofrnwhistler-mode chorus emissions by the four Clusterrnspacecraft during their first five years of operation. Thernresults can be divided into several broader categories. (I)rnSubstructure of chorus wave packets have been observedrnat time scales of 1–40 ms, with decreasing occurrencernrate for longer durations. Their growth rate is betweenrn30 and 400 s?1, and amplitudes reach up to 30 mV/mrnor 300 nT in the disturbed times. Maximum amplitudesrnare inside the larger chorus wave packets which occurrnat time scales above 100 ms. (ii) Frequency differencesrnhave been observed for chorus wave packets which werernsimultaneously detected by different spacecraft. Theserndifferences have been interpreted as differential Dopplerrnshift from rapidly moving elementary chorus sources atrnspeeds comparable to the parallel velocity of counterstreamingrnresonant electrons. (iii) At the altitude of thernperigee of Cluster satellites (≈4 Earth's radii), multipointrnmeasurement of the Poynting flux show that the centralrnposition of the chorus source region is located close to therngeomagnetic equatorial plane, fluctuating with amplitudernof u00193000 km and at speeds of the order of 100 km/s. Sizernof the source region along the field line, as obtained fromrnmultipoint measurement of electromagnetic planarity, isrn3000-5000 km. Multipoint correlation analysis of chorusrnwave packets has resulted in the size of the source regionrnof 100 km if measured perpendicular to the field line. (iv)rnStudies of propagation of chorus from its source regionrnshow that chorus can magnetospherically reflect and returnrnback to the equatorial plane at a lower altitude andrnwith a lower frequency than locally generated chorus. (v)rnComparison with nonlinear theory shows that many observedrnparameters of chorus emissions can be understoodrnon the basis of the backward wave oscillator model.
机译：我们总结了四个“群星”飞船在运行的前五年对惠斯勒模式合唱发射进行调查期间获得的结果。结果可以分为几大类。 （I）在1–40 ms的时间尺度上观察到了合唱波包的子结构，并在更长的时间内降低了发生率。它们的生长速度在30到400 s？1之间，并且在受干扰的时间内幅度达到30 mV / m或300 nT。最大振幅在较大的合唱波包内部，在超过100 ms的时间范围内出现。 （ii）已观察到由不同航天器同时检测到的合唱波包的频率差。这些差异已被解释为来自快速移动的基本合唱源的差分多普勒频移，其速度可与逆流共振电子的平行速度相媲美。 （iii）在星团卫星近地高处（地球半径约为4），对Poynting通量的多点测量表明，合唱源区的中心位置位于地磁赤道平面附近，并以振幅u00193000 km的速度波动。大约100 km / s。从电磁平面度的多点测量获得的沿磁力线的源区域的大小为3000-5000 km。如果垂直于磁力线测量，则合波包的多点相关分析导致源区域的大小为100 km。 （iv）对合唱团从其源区传播的研究表明，合唱团可以在较低的海拔高度以较低的频率和比本地产生的合唱团更低的频率磁层反射并返回赤道平面。 （v）与非线性理论的比较表明，在反向波振荡器模型的基础上，可以理解许多观察到的合唱发射参数。

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