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

被引:4
|
作者
Chmielewska, E. [1 ]
Tomczak, M. [1 ]
Kolomanski, S. [1 ]
Mrozek, T. [1 ,2 ]
机构
[1] Univ Wroclaw, Astron Inst, Wroclaw, Poland
[2] Polish Acad Sci, Space Res Ctr, Solar Phys Div, Warsaw, Poland
关键词
Sun: corona; Sun: coronal mass ejections (CMEs); Sun: flares; magnetic topology; CORONAL MASS EJECTIONS;
D O I
10.1002/asna.201612426
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
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
引用
收藏
页码:1016 / 1019
页数:4
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