SHINE: Understanding the Sun's Open Magnetic Flux

PI将结合数据分析和建模来调查太阳磁通量进入日光层的程度，以及这种磁通量在太阳周期过程中如何变化。他打算对Wang和Sheeley(1995)错误地将威尔逊山观测站校正因子应用于Wilcox太阳观测站磁图的猜想进行探讨。除其他问题外，PI计划研究行星际日冕物质抛射对行星际航天器在1AU处测量的磁通量的贡献，确定适用于各个太阳观测台的天气磁图的最佳修正因子，并推断这些结果对日冕磁通量传输和日光层磁通量积累理论的影响。PI声称，了解日冕的基本磁结构以及它是如何连接到日光层的，是最终预测空间天气影响的先决条件。该项目的目标直接解决了工作组在最近举行的2006年SIRE研讨会上提出的问题。

The PI will combine data analysis and modeling to investigate the degree to which the Sun's magnetic flux opens into the heliosphere and how this flux varies during the course of the solar cycle. He intends to explore the conjecture that Wang and Sheeley (1995) incorrectly applied the Mount Wilson Observatory correction factor to Wilcox Solar Observatory magnetograms. Among other issues, the PI plans to study the contribution of interplanetary CMEs to the magnetic flux measured at 1 AU by interplanetary spacecraft, to determine the best correction factors to apply to synoptic magnetograms from various solar observatories, and to deduce the implications of these results for theories of magnetic flux transport in the solar corona and the build-up of magnetic flux in the heliosphere.This research is relevant to the National Space Weather Program and SHINE. The PI asserts that understanding the basic magnetic structure of the solar corona and how it connects to the heliosphere is a prerequisite to eventually predicting space weather effects. The objectives of this project directly address questions raised by working group sessions at the recent 2006 SHINE workshop.