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首页> 外文期刊>Journal of Geophysical Research, A. Space Physics: JGR >Coronal mass ejection kinematics deduced from white light (Solar Mass Ejection Imager) and radio (Wind/WAVES) observations
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Coronal mass ejection kinematics deduced from white light (Solar Mass Ejection Imager) and radio (Wind/WAVES) observations

机译：从白光（Solar Mass Ejection Imager）和无线电（Wind / WAVES）观测结果推导出的冠状物质抛射运动学

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摘要

White-light and radio observations are combined to deduce the coronal and interplanetary kinematics of a fast coronal mass ejection (CME) that was ejected from the Sun at about 1700 UT on 2 November 2003. The CME, which was associated with an X8.3 solar flare from W56°, was observed by the Mauna Loa and Solar and Heliospheric Observatory (SOHO) Large-Angle Spectrometric Coronograph (LASCO) coronagraphs to 14 R . The measured plane-of-sky speed of the LASCO CME was 2600 km s?1. To deduce the kinematics of this CME, we use the plane-of-sky white light observations from both the Solar Mass Ejection Imager (SMEI) all-sky camera on board the Coriolis spacecraft and the SOHO/LASCO coronagraph, as well as the frequency drift rate of the low-frequency radio data and the results of the radio direction-finding analysis from the WAVES experiment on the Wind spacecraft. In agreement with the in situ observations for this event, we find that both the white light and radio observations indicate that the CME must have decelerated significantly beginning near the Sun and continuing well into the interplanetary medium. More specifically, by requiring self-consistency of all the available remote and in situ data, together with a simple, but not unreasonable, assumption about the general characteristic of the CME deceleration, we were able to deduce the radial speed and distance time profiles for this CME as it propagated from the Sun to 1 AU. The technique presented here, which is applicable to mutual SMEI/WAVES CME events, is expected to provide a more complete description and better quantitative understanding of how CMEs propagate through interplanetary space, as well as how the radio emissions, generated by propagating CME/shocks, relate to the shock and CME. This understanding can potentially lead to more accurate predictions for the onset times of space weather events, such as those that were observed during this unique period of intense solar activity.
机译：白光和射电观测相结合，推断出2003年11月2日大约1700 UT从太阳射出的快速日冕物质抛射（CME）的日冕和行星际运动学。与X8.3关联的CME莫纳罗阿火山和太阳与太阳大气观测站（SOHO）的大角度光谱日冕仪（LASCO）日冕仪观测到了W 56°的太阳耀斑，观测到14 R。测得的LASCO CME的天空平面速度为2600 km s？1。为了推论出这种CME的运动学，我们使用了科里奥利航天器和SOHO / LASCO日冕仪上太阳质量抛射成像仪（SMEI）全天候相机拍摄的天空平面白光观测值，以及频率风力飞行器的WAVES实验得出的低频无线电数据的漂移率和无线电测向分析的结果。与对此事件的现场观测结果一致，我们发现白光观测和无线电观测都表明CME必须从太阳附近开始并已经持续很好地进入行星际介质中了。更具体地说，通过要求所有可用的远程和原地数据的自洽性，以及对CME减速的一般特征的简单但并非不合理的假设，我们能够推算出CME减速的径向速度和距离时间曲线该CME从太阳传播到1 AU。此处介绍的技术适用于相互的SMEI / WAVES CME事件，有望对CME如何通过行星际空间传播以及通过传播CME /激波产生的无线电发射提供更完整的描述和更好的定量理解。 ，涉及到冲击和CME。这种理解可能会导致对空间天气事件的开始时间进行更准确的预测，例如在这一强烈的太阳活动独特时期所观察到的时间。

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