X-ray bright points (XBPs) in the coronal hole are often accompanied by out flows, while those in quiet region are not. Such a difference is important for understanding acceleration and mass supply to the solar wind. The purpose of this study is to compare the dynamics of bright points inside and outside polar coronal hole by using the same observing program.
Previous Hinode observations indicate XBPs fluctuate rapidly, which might be triggered by the interaction of magnetic field in the photosphere. Temporal variation of XBPs may also give us insights into the important question, whether the magnetism in polar region is the same as that in equatorial region or not. Time cadence is crucial for investigating temporal fluctuation. By employing interleaved sparse rasters, effective cadence of 6 minute can be achieved by EIS without compromising its spatial coverage. Coordination between Hinode and SUMER will provide comprehensive dataset ranging from the photosphere to the corona. |
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