  Arch-like loop structures filled with million Kelvin hot plasma form the
building blocks of the quiet-Sun corona. Both high-resolution observations and
magnetoconvection simulations show the ubiquitous presence of magnetic fields
on the solar surface on small spatial scales of $\sim$100\,km. However, the
question of how exactly these quiet-Sun coronal loops originate from the
photosphere and how the magnetic energy from the surface is channeled to heat
the overlying atmosphere is a long-standing puzzle. Here we report
high-resolution photospheric magnetic field and coronal data acquired during
the second science perihelion of Solar Orbiter that reveal a highly dynamic
magnetic landscape underlying the observed quiet-Sun corona. We found that
coronal loops often connect to surface regions that harbor fleeting weaker,
mixed-polarity magnetic field patches structured on small spatial scales, and
that coronal disturbances could emerge from these areas. We suggest that weaker
magnetic fields with fluxes as low as $10^{15}$\,Mx and/or those that evolve on
timescales less than 5\,minutes, are crucial to understand the coronal
structuring and dynamics.
