Correlation Between Coronal Mass Ejections And Solar Surface Activity

In this thesis, we summarized many kinds of activitives in solar atmosphere and presented the process of magnetic energy storage and release in solar activities. Meaningwhile, the space-borne and ground-based observations of the sun were introduced. In the main part of the thesis, the author's work were focused on the following points: 1, Reviewing present study condition and existing questions on the correlation between coronal mass ejection (CME) and solar surface activity; 2, Using the data observed by the SOHO (Solar and Heliospheric Observatory) from March 1997 to Dec. 2001, we study the correlations between the frontside halo CME and solar surface activity, some new results were: 1)> All 197 frontside halo CME observed by LASCO have close correlations with either flares or filament eruptions or oth; 2 All the CME were accompanied by localized brightening in chromosphere or low coronal inside their source regions. But sometimes such brightening was too weak to be called flares, or else all the CME were associated with flares; 3)^ About 78% of the halo CMEs were definitively correlated with eruptive flares; 4^ Almost 80% of the halo CME had their source regions inside active regions; 5)^ As to the spatial distributions between CME span extents and solar activities, half of the events were asymmetrical; 6)> Among these halo CMEs associated with GOES X-ray flares, 59% of the CMEs appeared prior to the onsets of flares, while 41%, after their disk counterparts. These results imply that CMEs have close correlations with solar activity, but such correlations are not 'cause and effect'. Plasma ejecta in flare and the opening of magnetic force line are of great importance to CME onset. Complex magnetic topology helps to trigger a CME. Since no CME theory model can explain the correlation between CME and surface activity, a new theory is needed strongly. 3. Integrating 26,624 pairs of video frames, we have mapped the circular polarization in an active-region filament against the solar disk bytraditional magnetograph working at HP line at Huairou Solar Observing Station. This filament offset the disc center, appeared at the boundary of three decayed active regions. It was quiet and away from any strong enhanced network. The mapped circular polarization in the filament has an average plarization degree of 1.1 * 10-3 with the measurement precision of 4 x 10-4. The mapping of circular polarization in filament may provide a supplementary diagnosis of filament magnetic field, in addition to the mapping of linear polarization via Hanle effects. However, the interpretation of the circular polarization appeals for the treatment of full quantum problem on Zeeman and non-Zeeman effects of Stokes line profiles.