The structure of magnetic flux ropes injected into the solar wind during
reconnection in the coronal atmosphere is explored with particle-in-cell
simulations and compared with {\it in situ} measurements of magnetic
"switchbacks" from the Parker Solar Probe. We suggest that multi-x-line
reconnection between open and closed flux in the corona will inject flux ropes
into the solar wind and that these flux ropes can convect outward over long
distances before disintegrating. Simulations that explore the magnetic
structure of flux ropes in the solar wind reproduce key features of the
"switchback" observations: a rapid rotation of the radial magnetic field into
the transverse direction (a consequence of reconnection with a strong guide
field); and the potential to reverse the radial field component. The potential
implication of the injection of large numbers of flux ropes in the coronal
atmosphere for understanding the generation of the solar wind is discussed.