U.S.-China Cooperative Research (Astronomy): Joint Observa- tions of the Long-Term Evolution of Solar Magnetic Fields

关于“联合观察气候变化的长期演变"的提案 哈罗德·齐林博士和肯·G。 加州理工学院的利布雷希特和艾未未教授 北京天文台的郭翔、韩峰、刘建强 天文台，由NSF和中国科学院联合赞助 科学。 在任何时候太阳都被弱磁场所覆盖 以30公里宽的元素网络的形式存在， 由大规模对流模式产生。 试图测量 磁网络的寿命表明， 元素持续约50小时。 当它们灭绝时，什么来代替它们 并不明显。 不幸的是，研究表明， 在24小时中，只有10个小时提供了良好的数据， 这些移动元素的来源可能是什么。 调查人员认为，解决这一问题的唯一办法是 对这些磁场进行连续观测。 在 目前，只有大熊太阳能的视频磁力仪 天文台和怀柔太阳天文台可以执行这一任务 任务 该计划将利用这两个网站的综合能力 每天24小时中的16小时， 的领域。 通过补充巡逻队的数据 望远镜在特拉维夫，调查人员应能够遵循 小磁场在几个24小时周期内的演化 并确定它们是如何进化的，从而实现一个新的 对太阳磁场特征的理解 服从。

This proposal on "Joint Observations of the Long Term Evolution of Solar Magnetic Fields" between Dr. Harold Zirin and Dr. Ken G. Libbrecht of California Institute of Technology and Professors Ai Guoxiang, Han Feng, and Liu Jianqiang of the Beijing Astronomical Observatory, is jointly sponsored by NSF and by the Chinese Academy of Sciences. At all times the sun is covered with weak magnetic fields arranged in the form of a network of elements 30 km across, thought to be generated by a large scale convective pattern. Attempts to measure the lifetime of the magnetic network have indicated that the elements last about 50 hours. What replaces them when they die out is not obvious. Unfortunately, studies from short daily runs provide good data for only 10 out of 24 hours, and do not show what the source of these moving elements might be. The investigators believe the only solution for this problem is to obtain continuous observations of these magnetic fields. At present, only the videomagnetographs of the Big Bear Solar Observatory and the Huairou Solar Observatory can perform this task. The program will use the combined capability of the two sites to cover 16 of 24 hours per day to follow the development and motion of the fields. By supplementing this with data from a patrol telescope in Tel Aviv, the investigators shall be able to follow the evolution of the small magnetic fields for several 24 hour periods and determine exactly how they evolve, thus achieving a new understanding of the magnetic features which underlie solar prominences.