估算晕日冕物质抛射宽度、震源位置和速度的一种新可能性
A new possibility to estimate the width, source location and velocity of halo CMEs
摘要：
晕日冕物质抛射的日冕照相观测受投影效应的影响是众所周知的。在天空的平面上观察不允许我们确定定义CME的geoeffectivness的关键参数，例如速度，宽度或源位置。我们假设晕日冕物质抛射在传播的开始阶段有恒定的速度，是对称的，传播与恒定的角宽度。利用这些近似，并确定投影速度和时间之间的差异，当CME出现在掩星盘的相对两侧，我们能够得到必要的参数。本文讨论了SOHO/LASCO星表中到2000年底的所有晕日冕物质抛射。我们表明，晕CME的平均速度更快，更广泛的比所有CME从SOHO/LASCO目录。
英文摘要：
It is well know that the coronagraphic observations of halo CMEs are subject to projection effects. Viewing in the plane of the sky does not allow us to determine the crucial parameters defining geoeffectivness of CMEs, such as the velocity, width or source location. We assume that halo CMEs at the beginning phase of propagation have constant velocities, are symmetric and propagate with constant angular widths. Using these approximations and determining projected velocities and difference between times when CME appears on the opposite sides of the occulting disk we are able to get the necessary parameters. We present consideration for the whole halo CMEs from SOHO/LASCO catalog until the end of 2000. We show that the halo CMEs are in average much more faster and wider than the all CMEs from the SOHO/LASCO catalog.
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