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首页> 外文期刊>Journal of Geophysical Research, A. Space Physics: JGR >Auroral signatures of the plasma injection and dipolarization in the inner magnetosphere
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Auroral signatures of the plasma injection and dipolarization in the inner magnetosphere

机译:极光的等离子体注入和签名dipolarization内部磁气圈

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Using auroral TV data and particle precipitation data from low-altitude satellites, weidentify the ionospheric signature of magnetotail dipolarizations and substorm injectionsmeasured in the near-Earth near-equatorial plasma sheet by Time History of Eventsand Macroscale Interactions during Substorms (THEMIS). Field line mapping exploits arecently developed time-dependent adaptive model which minimizes the variance toTHEMIS in situ magnetotail observations. We present strong evidence that theequatorward edge of the auroral bulge corresponds to the innermost extent of earthwardpropagating dipolarization fronts in the magnetosphere, whereas individual equatorwardmoving auroral enhancements correspond to the motion of individual injection frontsreaching at times distances as close to Earth as 5.5 RE. The region of tail dipolarizationcorresponds to the auroral bulge, a broad spatial region of enhanced but structuredauroral emissions, bounded on the poleward side by discrete auroral forms and on theequatorward side by a sharp drop in auroral luminosity and particle precipitation. Particleprecipitation within the bulge is enhanced considerably at the energies above 30 keV.Ionospheric protons are isotropic and electrons are anisotropic but with fluctuating fluxeswhich are below, but on occasion comparable with, trapped levels. The equatorwardedge of the bulge, herein termed the "Equatorward edge of Auroral Bulge" propagatesduring substorm expansion toward lower latitudes, initially fast (corresponding to 100 km/sin space at r ~ 7 RE) but with decreasing speed after onset. Our adaptive model mappingsuggests that equatorial points at near-geosynchronous altitude can map to ionosphericmagnetic latitudes up to 2°-3° off of predictions using standard T96 models. The offsetscan be either toward lower latitudes due to field line stretching before auroral breakup ortoward higher latitudes after breakup due to the near-Earth tail dipolarization.
机译:使用极光电视数据和粒子沉淀数据从低空卫星,weidentify电离层磁尾的签名dipolarizations和亚暴injectionsmeasured在近地近赤道等离子板时间事件和宏观尺度相互作用的历史在亚暴(裁判)。利用研究开发时间自适应模型,最小方差toTHEMIS原位磁尾观测。提出强有力的证据表明theequatorward边缘极光的凸起对应于最里面的程度earthwardpropagating dipolarization在磁气圈方面,而个人equatorwardmoving极光增强相对应个人的运动注入frontsreaching有时距离接近地球5.5再保险。该地区的尾巴dipolarizationcorresponds极光隆起,a广泛的增强,但空间区域structuredauroral排放,有界的向极一侧通过离散极光形式theequatorward极光急剧下降光度和粒子沉淀。Particleprecipitation内隆起大大增强能量超过30凯文。电子是各向异性,但波动fluxeswhich下面,但有时可比性,被困的水平。膨胀,此称为“朝赤道方向的边缘极光隆起”propagatesduring亚暴对低纬度地区扩张,最初快(对应于100公里/罪恶空间在r ~ 7再保险)但在开始以递减的速度。自适应模型mappingsuggests赤道点near-geosynchronous高度可以映射到ionosphericmagnetic纬度的2°3°使用标准T96模型预测。offsetscan是向低纬度地区极光分手前现场线拉伸分手是因为后ortoward高纬度地区近地尾dipolarization。

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