Modeling the distribution of magnetic fluxes in field concentrations in a solar active region
Modeling the distribution of magnetic fluxes in field concentrations in a solar active region
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模拟太阳活动区域磁场集中的磁通量分布
DOI：
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发表时间：
1997
期刊：
影响因子：
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通讯作者：
R. Shine
中科院分区：
文献类型：
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作者：
C. Schrijver;A. Title;H. Hagenaar;R. Shine
太阳和恒星光球层中的大部分磁场被排列成“通量管”簇，即，聚集成紧凑的区域，其中固有场强约为千高斯。通量浓度不断演变，因为它们与其他浓度合并或湮灭，或分裂成更小的浓度。这些过程导致形成包含广泛不同通量的浓度。Schrijver等人（1997年，论文I）为这种通量分布开发了一个统计模型，并在安静太阳的数据上进行了测试。在本文中，我们应用该模型的平均绝对通量密度是25倍以上的安静的网络研究论文I的磁谱。模型结果与观测到的谱区分布相当准确。决定分布函数形式的模型参数是碎裂参数与碰撞参数之比。我们得出结论，这个比例是相同的磁谱区和安静的网络。我们讨论了（近）表面对流的影响，以及该模型的适用性，恒星以外的太阳和输入的日冕加热的研究。
Much of the magnetic field in solar and stellar photospheres is arranged into clusters of ‘flux tubes’, i.e., clustered into compact areas in which the intrinsic field strength is approximately a kilogauss. The flux concentrations are constantly evolving as they merge with or annihilate against other concentrations, or fragment into smaller concentrations. These processes result in the formation of concentrations containing widely different fluxes. Schrijver et al. (1997, Paper I) developed a statistical model for this distribution of fluxes, and tested it on data for the quiet Sun. In this paper we apply that model to a magnetic plage with an average absolute flux density that is 25 times higher than that of the quiet network studied in Paper I. The model result matches the observed distribution for the plage region quite accurately. The model parameter that determines the functional form of the distribution is the ratio of the fragmentation and collision parameters. We conclude that this ratio is the same in the magnetic plage and in quiet network. We discuss the implications of this for (near-)surface convection, and the applicability of the model to stars other than the Sun and as input to the study of coronal heating.