Investigating the magnetic field of the quiet Sun internetwork

IF 2.2 4区 物理与天体物理 Q2 ASTRONOMY & ASTROPHYSICS
Mohamed Sedik, Abdelrazek M K Shaltout, Yuanyong Deng, Kiyoshi Ichimoto
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Abstract

Abstract We analyze the magnetism of the quiet Sun internetwork (IN) using high-spatial-resolution data obtained by the spectropolarimeter (SP) of the Solar Optical Telescope aboard the Hinode satellite near the disk center of the Sun. The SP data were inverted using the Stokes Inversion based on Response functions (SIR) inversion code with a single-component atmosphere with depth dependent in the solar photosphere, assuming gradients in physical parameters along the line of sight (LOS). To avoid the effect of noise, only pixels with Stokes U and/or Q signals above 4.5 times the noise level are considered. The inversion results show that the magnetic field of the IN has mainly hG field strength and the inclination distribution is quasi-isotropic at the solar surface. The field strength decreases with height and becomes predominantly horizontal at the upper layers. At the mid photosphere, the distributions of field strength and inclination are consistent with those derived by Milne–Eddington inversion. The mean transverse and longitudinal flux densities are 66 Mx cm−2 and 13 Mx cm−2 at log τ = −1.0; we also study the ratio between the transverse and longitudinal components in the IN region as a function of depth in the photosphere, finding that the ratio is almost 2.7 in the deep layer, increasing to 5.1 in the upper layer. The mean field strength is greater than 100 G in the upper photosphere, which is consistent with the results based on the Hanle effect. We present the LOS velocity probability distribution function for IN at different optical depths, where its distribution is mainly associated with upflow velocities of VLOS = 1.2 and 0.6 km s−1 in the deeper and upper layers, respectively. In addition, there exists a reliable inversion analysis, which is obvious from the comparison between the observed and calculated area asymmetries in both Fe i lines of Hinode SP data.
研究宁静太阳网络的磁场
摘要利用太阳光学望远镜的偏振光谱仪(SP)获得的高空间分辨率数据,分析了安静太阳网络(IN)的磁性。SP数据的反演采用基于响应函数(SIR)反演代码的Stokes反演,反演条件为单组分大气,大气深度依赖于太阳光球层,假设物理参数沿视线(LOS)方向存在梯度。为了避免噪声的影响,只考虑Stokes U和/或Q信号高于噪声水平4.5倍的像素。反演结果表明,太阳磁场以hG场强为主,太阳表面的倾角分布呈准各向同性。场强随高度的增加而减小,在上层以水平场强为主。在光球中部,场强和倾斜度的分布与Milne-Eddington反演结果一致。在log τ = - 1.0时,平均横向通量密度为66 Mx cm−2,纵向通量密度为13 Mx cm−2;我们还研究了in区域的横向分量与纵向分量之比和光球深度的关系,发现该比值在深层几乎为2.7,在上层增加到5.1。上层光球的平均场强大于100 G,这与基于汉勒效应的结果一致。我们给出了不同光学深度下IN的LOS速度概率分布函数,其分布主要与深部和上层VLOS分别为1.2和0.6 km s−1的上流速度有关。此外,从Hinode SP数据的两条Fe - i线的观测和计算面积不对称的对比中可以明显看出,存在可靠的反演分析。
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来源期刊
Publications of the Astronomical Society of Japan
Publications of the Astronomical Society of Japan 地学天文-天文与天体物理
CiteScore
4.10
自引率
13.00%
发文量
98
审稿时长
4-8 weeks
期刊介绍: Publications of the Astronomical Society of Japan (PASJ) publishes the results of original research in all aspects of astronomy, astrophysics, and fields closely related to them.
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