  The corona is a structure possessed by stars, including the sun. The abnormal
heating of the solar corona and chromosphere is one of the greatest mysteries
in modern astronomy. While state-of-the-art observations have identified some
candidates of magnetic activity events that could be responsible for this
abnormal heating, and theoretical studies have proposed various heating modes,
a complete physical picture of how they are heated as a whole remains elusive.
In this study, the characteristics of the heated corona and chromosphere are
investigated, and for the first time, the question of how they are abnormally
heated is explicitly answered by analyzing the long-term observations of the
global chromosphere in the Ca II K line and the global corona in the coronal
green line. The findings reveal that both the quiet chromosphere and corona are
in anti-phase with the solar cycle, whereas the active chromosphere and corona
are in phase with it. Different parts of the solar corona and chromosphere
exhibit significantly different variation characteristics, and are found to be
heated by different magnetic categories and probably in different modes. This
study posits that unraveling the heating mystery is best approached through the
lens of magnetic categories, rather than magnetic activity events.
