Full Stokes-vector inversion of the solar Mg II h & k lines

Hao Li, Tanausú del Pino Alemán, Javier Trujillo Bueno
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引用次数: 0

Abstract

The polarization of the Mg II h & k resonance lines is the result of the joint action of scattering processes and the magnetic field induced Hanle, Zeeman, and magneto-optical effects, thus holding significant potential for the diagnostic of the magnetic field in the solar chromosphere. The Chromospheric LAyer Spectro-Polarimeter sounding rocket experiment, carried out in 2019, successfully measured at each position along the 196 arcsec spectrograph slit the wavelength variation of the four Stokes parameters in the spectral region of this doublet around 280 nm, both in an active region plage and in a quiet region close to the limb. We consider some of these CLASP2 Stokes profiles and apply to them the recently-developed HanleRT Tenerife Inversion Code, which assumes a one-dimensional model atmosphere for each spatial pixel under consideration (i.e., it neglects the effects of horizontal radiative transfer). We find that the non-magnetic causes of symmetry breaking, due to the horizontal inhomogeneities and the gradients of the horizontal components of the macroscopic velocity in the solar atmosphere, have a significant impact on the linear polarization profiles. By introducing such non-magnetic causes of symmetry breaking as parameters in our inversion code, we can successfully fit the Stokes profiles and provide an estimation of the magnetic field vector. For example, in the quiet region pixels, where no circular polarization signal is detected, we find that the magnetic field strength in the upper chromosphere varies between 1 and 20 gauss.
太阳镁 II h 和 k 线的全斯托克斯向量反演
Mg II h和k共振线的偏振是散射过程和磁场诱导的汉勒、泽曼和磁光效应共同作用的结果,因此在诊断太阳色球层磁场方面具有重要潜力。2019年进行的色球层激光分光极谱仪探空火箭实验在196角秒光谱仪狭缝的每个位置都成功地测量了280纳米左右该双色球光谱区域内四个斯托克斯参数的波长变化,无论是在活跃区域的平台还是在靠近边缘的安静区域。我们考虑了 CLASP2 中的一些斯托克斯剖面,并将最近开发的 HanleRT Tenerife 反演代码应用于这些剖面,该代码假定所考虑的每个空间像素都是一维模型大气(即忽略了水平辐射传递的影响)。我们发现,由于太阳大气中的水平不均匀性和宏观速度水平分量的梯度,对称性破缺的非磁性原因对线性极化剖面有重大影响。通过在反演代码中引入这些非磁性的对称性破缺原因作为参数,我们可以成功地拟合斯托克斯剖面,并提供磁场矢量的估计值。例如,在没有检测到圆极化信号的静区像素中,我们发现上色球层的磁场强度在 1 到 20 高斯之间变化。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
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