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>Generation of a burst of geomagnetic pulsations in the 1-3 Hz frequency range in the daytime sector as a result of dramatic increases in the solar wind dynamic pressure
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Generation of a burst of geomagnetic pulsations in the 1-3 Hz frequency range in the daytime sector as a result of dramatic increases in the solar wind dynamic pressure
The spatio-temporal evolution of geomagnetic pulsation bursts at frequencies of 1-3 Hz, observed at the Mondy (MLT ≈ 1200; M _(lat) = 46.8°; L = 2.16) and Borok (MLT ≈ 0820; M _(lat) = 54.0°; L = 2. 94) midlatitude observatories and Lovozero auroral observatory (MLT ≈ 0820; M _(lat) = 64.2°; L = 5.36), has been studied. The considered bursts were registered in daytime sector of the magnetosphere after sudden impulses (SIs) caused by dramatic increases in the solar wind dynamic pressure and registered on board the WIND satellite. The SI onset time corresponds to the Sc * time shown in the Geomagnetic Indices Bulletin. The possible relationship between the excitation of these bursts and the variations in the particle partial density in the range of energies 0.03-45 keV per unit charge has been studied. The bursts were registered on board the LANL geosynchronous satellites. A comparison of the particle partial density variations measured on the satellites and the variation temperature anisotropy (A = T _⊥/T {double pipe} ~(-1)) with the variations in the pulsation burst amplitude on the ground indicated that the partial density maximum and the minimum (A ≤ 0) of the electron temperature anisotropy index in the vicinity of local noon coincide in time with the pulsation generation instant. A comparison of the electron partial density variations on the LANL-1994 and LANL-97A geosynchronous satellites spaced in longitude and the spatio-temporal variations in the development of bursts make it possible to assume that 1-3 Hz geomagnetic pulsations are excited in the vicinity of local noon and subsequently propagate along the ionospheric waveguide.
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机译：在Mondy（MLT≈1200; M _（lat）= 46.8°; L = 2.16）和Borok（MLT≈0820; M _（lat） ）= 54.0°; L =2。94）已经研究了中纬度天文台和Lovozero极光天文台（MLT≈0820; M _（lat）= 64.2°; L = 5.36）。考虑到的爆发是在太阳风动压力急剧增加引起的突然脉冲（SI）之后在磁层的白天扇区中记录的，并记录在WIND卫星上。 SI的开始时间对应于《地磁指数公报》中显示的Sc *时间。研究了这些脉冲的激发与每单位电荷0.03-45 keV能量范围内的粒子部分密度变化之间的可能关系。突发记录在LANL地球同步卫星上。将卫星上测得的粒子部分密度变化与温度各向异性（A = T_⊥/ T {双管}〜（-1））与地面上的脉动猝发振幅变化进行比较，表明局部正午附近的电子温度各向异性指数的密度最大值和最小值（A≤0）与脉动产生时刻在时间上一致。通过比较经纬度分布的LANL-1994和LANL-97A地同步卫星上的电子部分密度变化以及爆发发展中的时空变化，可以假设附近激发了1-3 Hz地磁脉冲局部正午，然后沿电离层波导传播。
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