Spectropolarimetric Inversions of the Ca ii 8542 Å Line in an M-class Solar Flare
Spectropolarimetric Inversions of the Ca ii 8542 Å Line in an M-class Solar Flare
复制标题
M 级太阳耀斑中 Ca ii 8542 Å 谱线的分光偏振反演
DOI：
10.3847/1538-4357/aac26d
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发表时间：
2018
期刊：
影响因子：
--
通讯作者：
M. Carlsson
中科院分区：
文献类型：
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作者：
D. Kuridze;D. Kuridze;Vasco M. J. Henriques;Michail Mathioudakis;L. R. Voort;J. D. L. C. Rodríguez;M. Carlsson
我们研究了M1.9级太阳耀斑SOL 2015 -09- 27 T10：40 UT，使用瑞典1米太阳望远镜CRISP成像分光偏振仪获得的Ca ii 8542线的高分辨率全斯托克斯成像分光偏振测量。光谱偏振反演使用非LTE代码NICOLE被用来构建半经验模型的耀斑大气调查的结构和演变的耀斑温度和磁场。耀斑区和非耀斑区温度分层的比较表明，耀斑带在耀斑峰期有很强的加热作用。在耀斑最大期间色球层中的带状物的偏振信号变得更强时，相比于其周围环境和前和后耀斑配置文件。此外，在耀斑和nonflaring的大气中的视线磁场和温度的扰动的响应函数的比较表明，在耀斑期间，Ca ii 8542线是更敏感的低层大气中的磁场预计将更强。色球磁场也确定了弱场近似，这导致与NICOLE反演得到的结果相似。
We study the M1.9-class solar flare SOL2015-09-27T10:40 UT using high-resolution full Stokes imaging spectropolarimetry of the Ca ii 8542 Å line obtained with the CRISP imaging spectropolarimeter at the Swedish 1-m Solar Telescope. Spectropolarimetric inversions using the non-LTE code NICOLE are used to construct semiempirical models of the flaring atmosphere to investigate the structure and evolution of the flare temperature and magnetic field. A comparison of the temperature stratification in flaring and nonflaring areas reveals strong heating of the flare ribbon during the flare peak. The polarization signals of the ribbon in the chromosphere during the flare maximum become stronger when compared to its surroundings and to pre- and post-flare profiles. Furthermore, a comparison of the response functions to perturbations in the line-of-sight magnetic field and temperature in flaring and nonflaring atmospheres shows that during the flare, the Ca ii 8542 Å line is more sensitive to the lower atmosphere where the magnetic field is expected to be stronger. The chromospheric magnetic field was also determined with the weak-field approximation, which led to results similar to those obtained with the NICOLE inversions.
DOI：
10.3847/0004-637x/827/2/101
发表时间：
2016-05
期刊：
The Astrophysical Journal
影响因子：
--
作者：
G. Kerr;L. Fletcher;A. Russell;J. Allred
通讯作者：
G. Kerr;L. Fletcher;A. Russell;J. Allred