Constraining Models of Coronal Mass Ejections (CMEs): Comparisons with Solar and In-Situ Observations

除了ACE和尤利西斯日冕物质抛射（cme）的现场测量外，还将使用日冕和内日球层的综合全球磁流体动力学（MHD）模型来解释SOHO和Yohkoh太阳观测。SAIC的全球模型将用于启动CME扰动并跟踪其演变至20个太阳半径。NOAA/SEC的日球层模型随后将在20个太阳半径处捕捉到这些结构，并将它们传播到5个天文单位。因此，将构建一个全球背景，其中可以将不同的太阳和原位观测联系起来。因此，提供了一个独特而有力的视角来解决有关日冕物质抛射的起源、磁拓扑和空间天气演变的基本问题。确定需要模拟的事件将由SHINE社区选择，模拟结果将在线向社区提供，以提高本次调查的科学回报。

A combined global magnetohydrodynamic (MHD) model of the solar corona and inner heliosphere will be used to interpret SOHO and Yohkoh solar observations in addition to ACE and Ulysses in-situ measurements of coronal mass ejections (CMEs). SAIC's global model will be employed to initiate the CME disturbance and follow its evolution out to 20 solar radii. NOAA/SEC's heliospheric model will subsequently pick up these structures at 20 solar radii and propagate them out to 5 AU. Thus a global context will be constructed wherein one may connect the disparate solar and in situ observations. A unique and powerful perspective is thus provided to address fundamental issues concerning the origin, magnetic topology, and space weather evolution of CMEs. The events identified for simulation are to be selected by the SHINE community, and the simulation results will be available to the community on-line, in order to enhance the scientific return of this investigation.