MILOS和MERLIN反演的极磁场与Hinode/SOT-SP数据的比较

IF 2.7 3区 物理与天体物理 Q2 ASTRONOMY & ASTROPHYSICS
Masahito Kubo, Daikou Shiota, Yukio Katsukawa, Masumi Shimojo, David Orozco Suárez, Nariaki Nitta, Marc DeRosa, Rebecca Centeno, Haruhisa Iijima, Takuma Matsumoto, Satoshi Masuda
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引用次数: 0

摘要

对极磁场及其时间演化的详细研究是日出的主要成果之一。对极磁场的精确测量对于理解太阳活动周期至关重要,因为它们为确定太阳风的来源区域提供了重要的约束条件。日野号上的太阳光学望远镜(SOT)的分光偏振计(SP)是最适合进行这种测量的仪器。在这项研究中,我们比较了极地地区的SOT-SP数据,使用两个具有代表性的Milne-Eddington反演代码MILOS和MERLIN进行处理。这些代码应用于相同的1级SOT-SP数据,并且在经过两次反转的地图上使用相同的消歧算法。我们发现MERLIN反演得到的径向磁通密度(相对于局部垂直方向的磁通密度)比MILOS反演得到的要大大约7% - 10%。在太阳活动周期的不同阶段观测到的极磁场中,MERLIN产生的略高的径向磁通量密度似乎是共同的。在MERLIN反演得到的散射光剖面和磁填充系数相同的条件下运行MILOS时,两种反演得到的径向磁通密度几乎相同。我们将径向磁通量密度的差异归因于两种反演所采用的不同填充因子,基于散射光剖面是在邻近像素上平均还是在整个视场上平均。由于横向磁场分量可能对径向磁通密度的估计有贡献,因此在极(边)观测中,径向磁通密度与磁填充因子之间的关系可能更为复杂。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
Comparison of Polar Magnetic Fields Derived from MILOS and MERLIN Inversions with Hinode/SOT-SP Data

The detailed investigation of the polar magnetic field and its time evolution is one of the major achievements of Hinode. Precise measurements of the polar magnetic field are essential for understanding the solar cycle, as they provide important constraints for identifying the source regions of the solar wind. The Spectropolarimeter (SP) of the Solar Optical Telescope (SOT) on board Hinode has been the instrument best suited to make such measurements. In this study, we compare the SOT-SP data for the polar regions, processed using two representative Milne-Eddington inversion codes, MILOS and MERLIN. These codes are applied to the same level-1 SOT-SP data, and the same disambiguation algorithm is used on the maps that go through the two inversions. We find that the radial magnetic-flux density (the magnetic-flux density with respect to the local vertical) provided by the MERLIN inversion tends to be approximately 7% – 10% larger than that obtained from the MILOS inversion. The slightly higher radial magnetic-flux density from MERLIN appears to be common to the polar magnetic fields observed at different phases of the solar cycle. When MILOS is run with the same scattered-light profile and the same magnetic filling factor that are derived with the MERLIN inversion, the radial magnetic-flux density derived from the two inversions is almost the same. We attribute the difference in the radial magnetic-flux density to different filling factors adopted by the two inversions, based on whether the scattered-light profiles are assumed to be the Stokes I profiles averaged over the neighboring pixels or over the entire field of view. The relationship between the radial magnetic-flux density and magnetic filling factor could be more complex in the polar (limb) observations due to the possible contributions of the transverse magnetic-field component to the estimation of the radial magnetic-flux density.

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来源期刊
Solar Physics
Solar Physics 地学天文-天文与天体物理
CiteScore
5.10
自引率
17.90%
发文量
146
审稿时长
1 months
期刊介绍: Solar Physics was founded in 1967 and is the principal journal for the publication of the results of fundamental research on the Sun. The journal treats all aspects of solar physics, ranging from the internal structure of the Sun and its evolution to the outer corona and solar wind in interplanetary space. Papers on solar-terrestrial physics and on stellar research are also published when their results have a direct bearing on our understanding of the Sun.
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