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Plasma diagnostics in two kinematic classes of CMEs observed by the Atmospheric Imaging Assembly onboard the Solar Dynamic Observatory

机译:太阳动力天文台上的大气成像组件观测到的两种运动学类别的CME的等离子体诊断

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In order to study the dynamics and thermal properties of two kinematic classes of coronal mass ejections (CMEs) we analyzed two well-observed events in the early stage of their propagation, using multiwavelength observations from the Atmospheric Imaging Assembly (AIA) of the Solar Dynamic Observatory (SDO). For deriving differential emission measure (DEM) profiles and DEM maps of the basic structures of CMEs, we used two methods: the regularized inversion and the iterative forward-fitting approach. For the CME associated with a M2.0 class flare (CME-FL), we identified a hot, moving, blob-like feature which seems to be a candidate for a CME flux rope. Furthermore, an expanding system of loop and coronal dimming was clearly seen in AIA images. For the CME related to an eruptive prominence (CME-EP), we observed an eruptive plasmoid and a failed-eruption of cold plasma. However, we also recognized warm and hot moving signatures that revealed a multi-temperature nature of the eruptive prominence. Our main results are as follows: (a) An analysis of the examples of the two different kinematic classes of CMEs shows that despite the slight variations in the values of speeds and accelerations (CME-FL: v approximate to 174 km s(-1), a approximate to 350 ms(-2); CME-EP: v approximate to 135 km s(-1), a approximate to 160 ms(-2)) they present the same kinematic behavior; (b) in the field of view of the LASCO coronagraphs these two events have the similar, positive accelerations; (c) for both events we observed an impulsive acceleration phase (IAP); (d) the expanding structures seen in 171 angstrom, 193 angstrom, 211 angstrom in both events move faster than th; (e) the plasmoid core for the CME-FL is hot (8.0-15.8 MK); (f) the expanding blob and the hot structure in the prominence region for the CME-EP event have the similar temperature range (0.8-2.5 MK). (C) 2016 WILEY-VCH Verlag GmbH& Co. KGaA, Weinheim
机译:为了研究两种运动学类型的日冕物质抛射(CME)的动力学和热学性质,我们使用来自太阳动力学的大气成像组件(AIA)的多波长观测结果,分析了在其传播早期的两个观测良好的事件。天文台(SDO)。为了导出CME基本结构的差分发射量度(DEM)轮廓和DEM图,我们使用了两种方法:正则化反演和迭代正向拟合法。对于与M2.0级火炬(CME-FL)相关的CME,我们确定了一个热的,运动的,斑点状的特征,似乎是CME助焊剂绳索的候选者。此外,在AIA图像中清楚地看到了环形和冠状调光的扩展系统。对于与爆发隆起(CME-EP)相关的CME,我们观察到了爆发浆浆和冷血浆喷发失败。但是,我们也认识到温暖和热动的特征,揭示了爆发隆起的多温性。我们的主要结果如下:(a)对两种不同运动学类型的CME的示例进行分析表明,尽管速度和加速度值略有变化(CME-FL:v约为174 km s(-1 ),大约为350 ms(-2); CME-EP:v大约为135 km s(-1),大约为160 ms(-2)),它们表现出相同的运动学行为; (b)在LASCO日冕仪的视野中,这两个事件具有相似的正加速度; (c)对于这两个事件,我们都观察到了脉冲加速阶段(IAP); (d)在这两种情况下,在171埃,193埃,211埃中看到的膨胀结构的移动速度都比th快; (e)CME-FL的浆线核心很热(8.0-15.8 MK); (f)CME-EP事件的突出区域的膨胀斑点和热结构具有相似的温度范围(0.8-2.5 MK)。 (C)2016 WILEY-VCH Verlag GmbH&Co.KGaA,魏因海姆

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