  Super-Earths, objects slightly larger than Earth and slightly smaller than
Uranus, have found a special place in exoplanetary science. As a new class of
planetary bodies, these objects have challenged models of planet formation at
both ends of the spectrum and have triggered a great deal of research on the
composition and interior dynamics of rocky planets in connection to their
masses and radii. Being relatively easier to detect than an Earth-sized planet
at 1 AU around a G star, super-Earths have become the focus of worldwide
observational campaigns to search for habitable planets. With a range of masses
that allows these objects to retain moderate atmospheres and perhaps even plate
tectonics, super-Earths may be habitable if they maintain long-term orbits in
the habitable zones of their host stars. Given that in the past two years a few
such potentially habitable super-Earths have in fact been discovered, it is
necessary to develop a deep understanding of the formation and dynamical
evolution of these objects. This article reviews the current state of research
on the formation of super-Earths and discusses different models of their
formation and dynamical evolution.
