论文标题
在太阳周期25的最小和上升阶段的白光电晕状态25-与过去的周期进行比较
The State of the White-Light Corona over the Minimum and Ascending Phases of Solar Cycle 25 -- Comparison with Past Cycles
论文作者
论文摘要
我们根据SOHO/LASCO-C2 CORONAGRPAPH所确定的，根据其辐射的时间演变和冠状质量弹出（CME）的特性（CMES）的时间演变以及冠状质量弹出（CME）的特性（CMES）的特性。将这些演变与过去两个SC中确定的演变进行了比较。 K-corona的集成辐射率和CME的发生率紧密跟踪太阳能活动的指标/代理，显着地是辐射的总磁场和CME的无线电通量，所有这些都在SC 25的上升阶段急剧上升。这一增长比预计的QUASI相似的标准和24号的预期均高得多，并且是SC 25和24的25和24的速度，并且是25和24之间的速度。在SC 24和25的最小值期间，辐射达到了相同的基础水平，但是流媒体带的纬度范围有所不同，在最低限度的最小值期间是更平坦的，实际上与SC 23的最低最小值更相似。将SC 23和24的下降分支缩减导致SC 24的持续时间，类似于11.0年的持续时间，类似于Scot Numpot Numpot Numpot Numpot Numpot Numbers。相比之下，在SC 25的最低最小值中，CME的发生率的基本水平明显大于前两个最小值期间。南半球比北部的半球更为活跃，这与几个预测以及半球黑子数的当前演变相一致。在SC 25的早期阶段，CME的平均表观宽度和Halo CMES的数量保持相对较大，恒定水平，这意味着地球球中弱总压力的持续存在。对于太阳能轨道和帕克太阳能探头即将进行的观察，这些结果和电晕比预期的电晕的观点非常有前途。
We report on the state of the corona over the minimum and ascending phases of Solar Cycle (SC) 25 on the basis of the temporal evolutions of its radiance and of the properties of coronal mass ejections (CMEs) as determined from white-light observations performed by the SOHO/LASCO-C2 coronagraph. These evolutions are further compared with those determined during the past two SC. The integrated radiance of the K-corona and the occurrence rate of CMEs closely track the indices/proxies of solar activity, prominently the total magnetic field for the radiance and the radio flux for the CMEs, all undergoing a steep increase during the ascending phase of SC 25. This increase is much steeper than anticipated on the basis of the predicted quasi similarity between SC 25 and 24, and is confirmed by the recent evolution of the sunspot number. The radiance reached the same base level during the minima of SC 24 and 25, but the latitudinal extent of the streamer belt differed, being flatter during the latter minimum and in fact more similar to that of the minimum of SC 23. Phasing the descending branches of SC 23 and 24 led to a duration of SC 24 of 11.0 years, similar to that given by the sunspot number. In contrast, the base level of the occurrence rate of CMEs during the minimum of SC 25 was significantly larger than during the two previous minima. The southern hemisphere is conspicuously more active than the northern one in agreement with several predictions and the current evolution of the hemispheric sunspot numbers. The mean apparent width of CMEs and the number of halo CMEs remains at relatively large, constant levels throughout the early phase of SC 25 implying the persistence of weak total pressure in the heliosphere. These results and the perspective of a corona more active than anticipated are extremely promising for the forthcoming observations by Solar Orbiter and Parker Solar Probe.
