根据SECCHI COR资料对极地急流的粒子动力学分析
Particle kinetic analysis of a polar jet from SECCHI COR data
摘要：
目标。我们分析了日冕观测的极地射流观测的太阳地球连接日冕和日光层调查（SECCHI）仪器套件板载的日地关系天文台（STEREO）航天器。方法.在我们的分析中，我们比较了一个专用的动力学粒子模型的白光日冕图像中的射流的亮度分布。我们得到了一致的时间估计，射流从太阳表面发射和近似的初始速度分布在喷流源。该方法还允许我们检查动力学模型的一致性。在这第一个应用中，我们只考虑重力作为沿磁场作用在喷流粒子上的主导力。结果我们发现动力学模型很好地解释了观测到的亮度演化。导出的起始时间与EUVI望远镜在不同波长下的喷流观测结果一致。初始粒子速度分布拟合麦克斯韦分布，我们发现偏离麦克斯韦分布的高能量尾部。我们估计喷流的总电子含量在3.2 \times 1014和1.8 \times 1015 g之间。映射沿喷流轨迹的积分粒子数到其源区，并假设一个典型的源区尺寸，我们得到一个初始的电子密度之间的8 \times 109和5 \times 1010 cm-3，这是较低的日冕或上色球层的特征。喷流源区域中所有粒子的总动能为2.1 \times 1028至2.4 \times 1029 erg。
英文摘要：
Aims. We analyze coronagraph observations of a polar jet observed by the Sun Earth Connection Coronal and Heliospheric Investigation (SECCHI) instrument suite onboard the Solar TErrestrial RElations Observatory (STEREO) spacecraft. Methods. In our analysis we compare the brightness distribution of the jet in white-light coronagraph images with a dedicated kinetic particle model. We obtain a consistent estimate of the time that the jet was launched from the solar surface and an approximate initial velocity distribution in the jet source. The method also allows us to check the consistency of the kinetic model. In this first application, we consider only gravity as the dominant force on the jet particles along the magnetic field. Results. We find that the kinetic model explains the observed brightness evolution well. The derived initiation time is consistent with the jet observations by the EUVI telescope at various wavelengths. The initial particle velocity distribution is fitted by Maxwellian distributions and we find deviations of the high energy tail from the Maxwellian distributions. We estimate the jet's total electron content to have a mass between 3.2 \times 1014 and 1.8 \times 1015 g. Mapping the integrated particle number along the jet trajectory to its source region and assuming a typical source region size, we obtain an initial electron density between 8 \times 109 and 5 \times 1010 cm-3 that is characteristic for the lower corona or the upper chromosphere. The total kinetic energy of all particles in the jet source region amounts from 2.1 \times 1028 to 2.4 \times 1029 erg.
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