Formation of Near-Surface Magnetic Fields of the Sun

IF 0.7 4区 地球科学 Q4 GEOCHEMISTRY & GEOPHYSICS
A. G. Tlatov, I. A. Berezin, K. A. Tlatova
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Abstract

In this work, we studied the formation of a large-scale magnetic field. For this, we used the surface flux transport (SFT) model. We have studied the model’s accuracy and its sensitivity to uncertainties in its key parameters and input data. We also compared the simulated magnetic field with observations of the SDO/HMI and STOP/Kislovodsk magnetic fields. Overall there is good agreement between the simulations and observations. Although the model cannot reproduce fine details of the magnetic field, the long-term evolution of the polar field is very similar in simulations and observations. During even one activity cycle, large-scale field drift waves to high latitudes change polarity. Magnetic field drift waves, the sign of which corresponds to the magnetic polarity of the trailing parts of the active regions, often exist during the decline phase of activity. This does not quite correspond to the idea of mutual compensation of the leading fields of active regions across the equator. We also looked at the magnetic field flux across the equator. We confirmed that the flux across the equator does not show a clear predominance of leading sunspot polarity. The results are discussed to test dynamo models.

Abstract Image

太阳近表面磁场的形成
在这项工作中,我们研究了大尺度磁场的形成。为此,我们使用了表面通量输运(SFT)模型。研究了模型的精度及其对关键参数和输入数据不确定性的敏感性。我们还将模拟磁场与SDO/HMI和STOP/Kislovodsk的观测结果进行了比较。总的来说,模拟和观测结果吻合得很好。虽然该模型不能再现磁场的精细细节,但在模拟和观测中,极磁场的长期演变非常相似。即使在一个活动周期内,向高纬度地区的大尺度场漂移波也会改变极性。磁场漂移波的符号与活跃区尾部的磁极相对应,常在活跃区衰退期出现。这并不完全符合赤道上活跃区域的主要磁场相互补偿的想法。我们还研究了穿越赤道的磁场通量。我们证实,穿越赤道的通量并没有显示出太阳黑子极性的明显优势。对结果进行了讨论,以测试发电机模型。
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来源期刊
Geomagnetism and Aeronomy
Geomagnetism and Aeronomy Earth and Planetary Sciences-Space and Planetary Science
CiteScore
1.30
自引率
33.30%
发文量
65
审稿时长
4-8 weeks
期刊介绍: Geomagnetism and Aeronomy is a bimonthly periodical that covers the fields of interplanetary space; geoeffective solar events; the magnetosphere; the ionosphere; the upper and middle atmosphere; the action of solar variability and activity on atmospheric parameters and climate; the main magnetic field and its secular variations, excursion, and inversion; and other related topics.
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