  We present JWST images of the well-known planetary nebula NGC 6720 (the Ring
Nebula), covering wavelengths from 1.6$\mu$m to 25 $\mu$m. The bright shell is
strongly fragmented with some 20 000 dense globules, bright in H$_2$, with a
characteristic diameter of 0.2 arcsec and density $n_{\rm H} \sim 10^5$-$10^6$
cm$^{-3}$. The shell contains a thin ring of polycyclic aromatic hydrocarbon
(PAH) emission. H$_2$ is found throughout the shell and in the halo. H$_2$ in
the halo may be located on the swept-up walls of a biconal polar flow. The
central cavity is shown to be filled with high ionization gas and shows two
linear structures. The central star is located 2 arcsec from the emission
centroid of the cavity and shell. Linear features (`spikes') extend outward
from the ring, pointing away from the central star. Hydrodynamical simulations
are shown which reproduce the clumping and possibly the spikes. Around ten
low-contrast, regularly spaced concentric arc-like features are present; they
suggest orbital modulation by a low-mass companion with a period of about 280
yr. A previously known much wider companion is located at a projected
separation of about 15 000 au; we show that it is an M2-M4 dwarf. The system is
therefore a triple star. These features, including the multiplicity, are
similar to those seen in the Southern Ring Nebula (NGC 3132) and may be a
common aspect of such nebulae.
