• 主题
高级搜索  >
历史搜索 清空历史
首页> 外文期刊>Astronomy and astrophysics >Reconstructing solar magnetic fields from historical observations
【24h】

Reconstructing solar magnetic fields from historical observations

机译：从历史观察中重建太阳磁场

获取原文
           
页面导航
  • 摘要
  • 著录项
  • 相似文献
  • 相关主题

摘要

Aims . The evolution of the photospheric magnetic field has only been regularly observed since the 1970s. The absence of earlier observations severely limits our ability to understand the long-term evolution of solar magnetic fields, especially the polar fields that are important drivers of space weather. Here, we test the possibility to reconstruct the large-scale solar magnetic fields from Ca II K line observations and sunspot magnetic field observations, and to create synoptic maps of the photospheric magnetic field for times before modern-time magnetographic observations. Methods . We reconstructed active regions from Ca II K line synoptic maps and assigned them magnetic polarities using sunspot magnetic field observations. We used the reconstructed active regions as input in a surface flux transport simulation to produce synoptic maps of the photospheric magnetic field. We compared the simulated field with the observed field in 1975?1985 in order to test and validate our method. Results . The reconstruction very accurately reproduces the long-term evolution of the large-scale field, including the poleward flux surges and the strength of polar fields. The reconstruction has slightly less emerging flux because a few weak active regions are missing, but it includes the large active regions that are the most important for the large-scale evolution of the field. Although our reconstruction method is very robust, individual reconstructed active regions may be slightly inaccurate in terms of area, total flux, or polarity, which leads to some uncertainty in the simulation. However, due to the randomness of these inaccuracies and the lack of long-term memory in the simulation, these problems do not significantly affect the long-term evolution of the large-scale field.
机译：目的。自1970年代以来，仅定期观察到光球磁场的演变。缺乏早期观测资料严重限制了我们了解太阳磁场（尤其是构成太空天气的重要驱动因素的极性场）长期演变的能力。在这里，我们测试了从Ca II K线观测和黑子磁场观测重建大型太阳磁场的可能性，并创建了近现代磁成像观测之前的光球磁场概要地图。方法 。我们从Ca II K线天气图重建了活动区域，并使用黑子磁场观测为它们分配了磁极性。我们将重建的有源区域用作表面通量传输模拟中的输入，以生成光球磁场的天气图。为了比较和验证我们的方法，我们在1975？1985年将模拟场与观测场进行了比较。结果。重建过程非常准确地再现了大范围场的长期演变，包括极向磁通量浪涌和极场强度。由于缺少一些较弱的活动区域，因此重建的新兴通量略少，但其中包括对电场的大规模演化最重要的大型活动区域。尽管我们的重建方法非常健壮，但是单个重建的有源区域在面积，总通量或极性方面可能会略有误差，这会导致仿真中出现一些不确定性。但是，由于这些不精确性的随机性以及模拟中缺乏长期记忆，因此这些问题不会显着影响大范围场的长期演化。

著录项

相似文献

  • 外文文献
  • 中文文献
  • 专利
获取原文

客服邮箱：kefu@zhangqiaokeyan.com

京公网安备：11010802029741号 ICP备案号：京ICP备15016152号-6 六维联合信息科技 (北京) 有限公司©版权所有

  • 客服微信

  • 服务号