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Abnormal Stokes Profiles of the Photospheric Lines in the Region of Chromospheric Dual Flows in the Surroundings of a Solar Pore: 2. Photospheric Models
Kinematics and Physics of Celestial Bodies ( IF 0.5 ) Pub Date : 2018-08-30 , DOI: 10.3103/s0884591318040049
N. N. Kondrashova

Abstract

The thermodynamic parameters and parameters of the photospheric magnetic field in the region of chromospheric dual flows in the vicinity of a small pore in the active region NOAA 11024 are presented. The dual chromospheric flows that appeared in the region of abnormal Stokes V profiles of the photospheric lines were associated with the emergence of a new small-scale magnetic flux of positive polarity. Semiempirical photospheric models were obtained by inversion using the SIR program (Stokes Inversion based on Response functions) [42]. Each model contains two components: two thin magnetic flux tubes of different polarity. The magnetic flux has a negative polarity in the first component and positive in the second. The Stokes profiles of the photospheric lines Fe I λ 630.15, 630.25, and 630.35 nm and Ti I λ 630.38 nm from the spectropolarimetric observations with the French–Italian telescope THEMIS (Tenerife, Spain) were used for modeling. The altitudinal dependences of the temperature, line of sight velocity, inclination angle of the magnetic field vector, and azimuth angle in the tubes, as well as the values of the magnetic field strength and macroturbulent velocity, are obtained. The time variations in all parameters of the photosphere are revealed. The new magnetic flux emerged in the region of mixed polarities and was accompanied by the heating of the photosphere and chromosphere. The inferred flux tube models show the temperature enhancement by 400 K in the upper photospheric layers relative to the quiet-Sun model temperature. They indicate a complex, inhomogeneous small-scale structure of the magnetic field and the velocity field. The magnetic field strength in the tubes varies from 0.03 to 0.13 T during the period under consideration. The inclination angles of the magnetic field vector and the azimuth angles strongly differ in magnetic flux tubes and vary in time. The line-of-sight velocity does not exceed 2 km/s. The downflows in the lower layers of the photosphere and the upflows in the upper layers dominate in the first component of the models. In the second component of the model, the material in the upper photosphere is lifted. The macroturbulent velocity in most cases exceeds its value for the unperturbed photosphere. The velocity is greater in the second component of the models. The emergence of the new magnetic flux could lead to the magnetic reconnection and occurrence of a microflare.


中文翻译:

太阳孔隙环境中双峰流区域中光球线的异常斯托克斯曲线:2.光球模型

摘要

提出了热力学参数和在活动区NOAA 11024中小孔隙附近的色球双流区域中的光球磁场参数。在异常斯托克斯V区出现的双色球层流光球线的轮廓与新的正极性小规模磁通的出现有关。使用SIR程序(基于响应函数的斯托克斯反演)通过反演获得半经验光球模型[42]。每个模型包含两个组件:两个极性不同的细磁通管。磁通量在第一分量中具有负极性,在第二分量中具有正极性。使用法国-意大利望远镜THEMIS(西班牙特内里费岛)的分光偏振观测法对光球线Fe Iλ630.15、630.25和630.35 nm和Ti Iλ630.38 nm的斯托克斯轮廓进行建模。温度,视线速度,磁场矢量的倾斜角和管中的方位角的高度依赖性,以及磁场强度和大湍流速度的值。揭示了光球所有参数的时间变化。新的磁通量出现在混合极性区域,并伴有光球和色球的加热。推断的通量管模型显示出,相对于安静太阳模型温度,上部光层的温度提高了400K。它们表明了磁场和速度场的复杂,不均匀的小尺度结构。在所考虑的时间内,管中的磁场强度从0.03到0.13 T不等。磁场矢量的倾斜角和方位角在磁通管中差异很大,并且随时间变化。视线速度不超过2 km / s。在模型的第一个组成部分中,光层较低层的向下流动和较高层的向上流动占主导地位。在模型的第二个组件中,上部光球中的材料被提升。在大多数情况下,宏观湍流速度超过其在未受干扰的光球中的值。在模型的第二部分,速度更大。新的磁通量的出现可能导致磁重新连接并出现微光斑。
更新日期:2018-08-30
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