A statistical study on the brightening propagation of post-flare loops  

作　　者：LI LePing DUAN HongYu ZHANG Jun 

机构地区：[1]Key Laboratory of Solar Activity,National Astronomical Observatories,Chinese Academy of Sciences,Beijing 100012,China [2]Jiangsu Sopo Corporation Group Ltd.,Zhenjiang 212006,China

出　　处：《Science China(Physics,Mechanics & Astronomy)》2009年第11期1723-1727,共5页中国科学：物理学、力学、天文学（英文版）

基　　金：Supported by the National Natural Science Foundation of China (Grant Nos. G10703007, 40890161, 10603008, 40674081, and 10733020);the CAS Project (Grant No. KJCX2-YW-T04);the National Basic Research Program of China (Grant No. G2006CB806303)

摘　　要：After examining the data observed by TRACE 171 and 195  from May 1998 to December 2006, we choose as our sample 190 (39 X-class and 151 M-class) flare events which display post-flare loops (PFLs). We investigate the brightening propagation of these PFLs of the events in the sample along the magnetic neutral lines. In most of the cases, the length of the flare ribbons (FRs) ranges from 20 to 170 Mm. The propagating duration of the brightening lasts 10-60 min. The velocities of the propagation associated with the flare strength and the length of the FRs, range from 5 to 35 km·s-1. Furthermore, a greater propagating velocity corresponds to a greater deceleration (or acceleration). These PFLs display three types of propagating patterns: (1) the brightening begins at the middle part of a set of PFLs, and propagates bi-directionally towards its both ends; (2) the brightening first appears at one end of a set of PFLs, and then propagates to the other; (3) the initial brightening takes place at two (or more than two) positions on two (or more than two) sets of PFLs, and each brightening propagates bi-directionally along the magnetic neutral line.After examining the data observed by TRACE 171 and 195 ? from May 1998 to December 2006, we choose as our sample 190 (39 X-class and 151 M-class) flare events which display post-flare loops (PFLs). We investigate the brightening propagation of these PFLs of the events in the sample along the magnetic neutral lines. In most of the cases, the length of the flare ribbons (FRs) ranges from 20 to 170 Mm. The propagating duration of the brightening lasts 10–60 min. The velocities of the propagation associated with the flare strength and the length of the FRs, range from 5 to 35 km·s?1. Furthermore, a greater propagating velocity corresponds to a greater deceleration (or acceleration). These PFLs display three types of propagating patterns: (1) the brightening begins at the middle part of a set of PFLs, and propagates bi-directionally towards its both ends; (2) the brightening first appears at one end of a set of PFLs, and then propagates to the other; (3) the initial brightening takes place at two (or more than two) positions on two (or more than two) sets of PFLs, and each brightening propagates bi-directionally along the magnetic neutral line.

关 键 词：FLARES magnetic FIELDS CORONA UV radiation 

分 类 号：P182.52[天文地球—天文学]