Studying the behavior of coronal mass ejections (CMEs) is important for both solar physics and space weather. The correlations of smoothed monthly mean daily integrated CME acceleration [\(a\)], mass [\(M\)], and the force [\(Ma\)] to drive CMEs with sunspot activity [\(R_{\mathrm{I}}\)] are analyzed for both slow and fast CMEs and for both Solar Cycles 23 and 24 separately. It is found that \(a\) is inversely related to both \(R_{\mathrm{I}}\) and \(M\). The correlation between \(Ma\) and \(R_{\mathrm{I}}\) for both slow and fast CMEs is negative at the rising phase of Solar Cycle 23 and positive otherwise. There is a sharp peak in \(\gamma =Ma/R_{\mathrm{I}}\) near the solar minimum (December 2008) for both slow and fast CMEs. However, for fast CMEs, there is a sharp negative peak near the previous solar minimum (August 1996) and another positive peak near the current solar minimum (2019). The positive (negative) peak tends to be related to the solar minimum from a stronger (weaker) to a weaker (stronger) solar cycle. These results suggest that the CME acceleration depends more on the strength of solar activity than on the CME’s speed. Stronger magnetic activity may slow down the CMEs that are too massive or too fast and weaker activity may speed up the CMEs that are less massive or too slow. During a few years’ period of magnetic-field polarity reversal around the solar minimum, the force provided by large-scale magnetic-field structures may not be strong enough to constrain CME motions, leading to the “escape” of CMEs with large \(|\gamma |\).

研究日冕物质抛射（CME）的行为对于太阳物理学和太空天气都非常重要。平滑的月平均日均CME加速度[ \（a \） ]，质量[ \（M \） ]和驱动力[ \（Ma \） ]的相关性，以驱动具有黑子活动的CME [ \（R _ {\ mathrm {I}} \） ]分别针对慢速和快速CME以及太阳周期23和24进行了分析。发现\（a \）与\（R _ {\ mathrm {I}} \）和\（M \）都成反比。之间的相关性\（马\）和\（R _ {\ mathrm {I}} \）在太阳周期23的上升阶段，慢速和快速CME都为负，否则为正。\（\ gamma = Ma / R _ {\ mathrm {I}} \）中有一个尖峰慢速和快速CME均接近太阳最低值（2008年12月）。但是，对于快速的CME，在前一个太阳最低值附近（1996年8月）有一个急剧的负峰，在当前太阳最低值附近（2019年）有另一个正峰。正（负）峰值往往与太阳周期的最小值（从较强（较弱）到较弱（较强））有关。这些结果表明，CME的加速度更多地取决于太阳活动强度，而不是CME的速度。较强的磁活动可能会使过大或过快的CME变慢，而较弱的活动可能会使过少或过慢的CME加速。在围绕太阳极小值的磁场极性反转的几年期间，大型磁场结构提供的力可能不足以限制CME运动，\（| \ gamma | \）。