  We present EUV solar observations showing evidence for omnipresent jetting
activity driven by small-scale magnetic reconnection at the base of the solar
corona. We argue that the physical mechanism that heats and drives the solar
wind at its source is ubiquitous magnetic reconnection in the form of
small-scale jetting activity (i.e., a.k.a. jetlets). This jetting activity,
like the solar wind and the heating of the coronal plasma, are ubiquitous
regardless of the solar cycle phase. Each event arises from small-scale
reconnection of opposite polarity magnetic fields producing a short-lived jet
of hot plasma and Alfv\'en waves into the corona. The discrete nature of these
jetlet events leads to intermittent outflows from the corona, which homogenize
as they propagate away from the Sun and form the solar wind. This discovery
establishes the importance of small-scale magnetic reconnection in solar and
stellar atmospheres in understanding ubiquitous phenomena such as coronal
heating and solar wind acceleration. Based on previous analyses linking the
switchbacks to the magnetic network, we also argue that these new observations
might provide the link between the magnetic activity at the base of the corona
and the switchback solar wind phenomenon. These new observations need to be put
in the bigger picture of the role of magnetic reconnection and the diverse form
of jetting in the solar atmosphere.
