  The recent rediscovery of magnetic field switchbacks or deflections embedded
in the solar wind flow by the Parker Solar Probe mission lead to a huge
interest in the modelling of the formation mechanisms and origin of these
switchbacks. Several scenarios for their generation were put forth, ranging
from lower solar atmospheric origins by reconnection, to being a manifestation
of turbulence in the solar wind, and so on. Here we study some potential
formation mechanisms of magnetic switchbacks in the lower solar atmosphere,
using three-dimensional magneto-hydrodynamic (MHD) numerical simulations. The
model is that of an intense flux tube in an open magnetic field region, aiming
to represent a magnetic bright point opening up to an open coronal magnetic
field structure, e.g. a coronal hole. The model is driven with different plasma
flows in the photosphere, such as a fast up-shooting jet, as well as shearing
flows generated by vortex motions or torsional oscillations. In all scenarios
considered, we witness the formation of magnetic switchbacks in regions
corresponding to chromospheric heights. Therefore, photospheric plasma flows
around the foot-points of intense flux tubes appear to be suitable drivers for
the formation of magnetic switchbacks in the lower solar atmosphere.
Nevertheless, these switchbacks do not appear to be able to enter the coronal
heights of the simulation in the present model. In conclusion, based on the
presented simulations, switchbacks measured in the solar wind are unlikely to
originate from photospheric or chromospheric dynamics.
