The coronal heating problem is a long-standing perplexing issue. In this study, 13 solar activity indexes are used to investigate their phase relation with the sunspot number (SSN). Only three of them are found to statistically significantly lag the SSN (large-scale magnetic activity) by about one solar rotation period; the three indexes are total solar irradiance (TSI), the modified coronal index, and the solar wind velocity; the former two indexes may represent the long-term variation of energy quantity of the heated photosphere and corona, respectively. The Mount Wilson Sunspot Index (MWSI) and the Magnetic Plage Strength Index (MPSI), which reflect the large- and small-scale magnetic field activities, respectively, are also utilised to investigate their phase relations with the three indexes. The three indexes are found to be much more intimately related to MPSI than to MWSI, and MWSI statistically significantly leads TSI by about one rotation period. The heated corona is found to pulse perfectly in step with the small-scale magnetic activity rather than the large-scale magnetic activity; furthermore, combined with observations, our statistical evidence should thus attribute coronal heating firmly to small-scale magnetic activity phenomena, such as spicules, micro-flares, nano-flares, and others. The photosphere and the corona are synchronously heated, which should seemingly prefer magnetic reconnection heating to wave heating. In the long term, such a coronal heating way is inferred effective. Statistically, it is also small-scale magnetic activity phenomena that produce TSI enhancement. Coronal heating and solar wind acceleration are found to be synchronous, as standard models require.

中文翻译：

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通过太阳活动指数的相位关系研究日冕加热

日冕加热问题是一个长期存在的令人困惑的问题。在这项研究中，使用了 13 个太阳活动指数来研究它们与太阳黑子数 (SSN) 的相位关系。仅发现其中三个在统计上显着滞后于 SSN（大规模磁活动）约一个太阳自转周期；这三个指标是太阳总辐照度（TSI）、修正日冕指数和太阳风速；前两个指标可以分别代表受热光球和日冕能量的长期变化。分别反映大尺度和小尺度磁场活动的威尔逊山太阳黑子指数（MWSI）和磁斑强度指数（MPSI）也被用来研究它们与三个指数的相位关系。发现这三个指数与 MPSI 的关系比与 MWSI 的关系更密切，MWSI 在统计上显着领先于 TSI 大约一个轮换周期。发现加热的日冕与小规模的磁活动而不是大规模的磁活动完全同步；此外，结合观察，我们的统计证据应该将日冕加热牢固地归因于小尺度的磁活动现象，例如针状体、微耀斑、纳米耀斑等。光球和日冕是同步加热的，看起来应该更喜欢磁重联加热而不是波加热。从长远来看，这种日冕加热方式被推断是有效的。据统计，产生TSI增强的也是小尺度的磁活动现象。