FIRST DETECTION OF CHROMOSPHERIC MAGNETIC FIELD CHANGES DURING AN X1-FLARE
FIRST DETECTION OF CHROMOSPHERIC MAGNETIC FIELD CHANGES DURING AN X1-FLARE
复制标题
首次检测 X1 耀斑期间色球磁场变化
DOI：
--
复制
发表时间：
2016
期刊：
影响因子：
--
通讯作者：
L. Kleint
中科院分区：
文献类型：
--
作者：
L. Kleint
在许多耀斑期间，已经观察到光球磁场的阶梯式变化，它往往变得更加水平。以前的解释包括日冕环的收缩，并推测这种猛拉可能是造成太阳地震的原因。在这里，我们报告的逐步色球视线磁场（B）的变化，通过光谱偏振测量的Ca ii 8542在X1耀斑SOL 20140329 T17：48期间获得的DST/IBIS。这些变化更强（<640 Mx cm−2），并且比它们的光球对应物（<320 Mx cm−2）出现在更大的区域。的绝对值通常减少而不是增加。光球的变化主要发生在极性反转线附近，色球的变化主要发生在环的足点附近。变化的位置很近，但不完全是硬X射线发射的空间，既不是增强的连续发射，也不是一个小的太阳地震。色球和日冕的发射几乎在所有的位置都有增强，但也有许多位置的发射没有任何变化。光球层和色球层的变化在时间、符号和大小上表现出不同，似乎彼此独立。一个简单的收缩环模型产生的变化与观察到的相反。对这种差异的解释可能是增加环的大小或环在耀斑期间在某个方向上解旋。目前还不清楚是哪些过程导致了观测到的变化及其时间、大小和位置，特别是考虑到光球层和色球层之间的不相干性。
Stepwise changes of the photospheric magnetic field, which often becomes more horizontal, have been observed during many flares. Previous interpretations include coronal loops that contract, and it has been speculated that such jerks could be responsible for sunquakes. Here we report the detection of stepwise chromospheric line-of-sight magnetic field (B ) changes obtained through spectropolarimetry of Ca ii 8542 Å with DST/IBIS during the X1-flare SOL20140329T17:48. These changes are stronger (<640 Mx cm−2) and appear in larger areas than their photospheric counterparts (<320 Mx cm−2). The absolute value of more often decreases than increases. Photospheric changes are predominantly located near a polarity inversion line, and chromospheric changes near the footpoints of loops. The locations of changes are near, but not exactly co-spatial to hard X-ray emission and neither to enhanced continuum emission nor to a small sunquake. Enhanced chromospheric and coronal emission is observed in nearly all locations that exhibit changes of , but the emission also occurs in many locations without any changes. Photospheric and chromospheric changes of show differences in timing, sign, and size and seem independent of each other. A simple model of contracting loops yields changes of the opposite sign to those observed. An explanation for this discrepancy could be increasing loop sizes or loops that untwist in a certain direction during the flare. It is yet unclear which processes are responsible for the observed changes and their timing, size, and location, especially considering the incoherence between the photosphere and the chromosphere.
基于 SDO/HMI 观测的主要喷发活跃区磁场和能量的演化
DOI：
10.1088/0004-637x/748/2/77
发表时间：
2012
期刊：
The Astrophysical Journal
影响因子：
--
作者：
Hoeksema;Wiegelmann;T.Hayashi;Thalmann
通讯作者：
Thalmann