  Here we review the recent progress made in the detection, examination,
characterisation and interpretation of oscillations manifesting in small-scale
magnetic elements in the solar photosphere. This region of the Sun's atmosphere
is especially dynamic, and importantly, permeated with an abundance of magnetic
field concentrations. Such magnetic features can span diameters of hundreds to
many tens of thousands of km, and are thus commonly referred to as the
`building blocks' of the magnetic solar atmosphere. However, it is the smallest
magnetic elements that have risen to the forefront of solar physics research in
recent years. Structures, which include magnetic bright points, are often at
the diffraction limit of even the largest of solar telescopes. Importantly, it
is the improvements in facilities, instrumentation, imaging techniques and
processing algorithms during recent years that have allowed researchers to
examine the motions, dynamics and evolution of such features on the smallest
spatial and temporal scales to date. It is clear that while these structures
may demonstrate significant magnetic field strengths, their small sizes make
them prone to the buffeting supplied by the ubiquitous surrounding convective
plasma motions. Here, it is believed that magnetohydrodynamic waves can be
induced, which propagate along the field lines, carrying energy upwards to the
outermost extremities of the solar corona. Such wave phenomena can exist in a
variety of guises, including fast and slow magneto-acoustic modes, in addition
to Alfven waves. Coupled with rapid advancements in magnetohydrodynamic wave
theory, we are now in an ideal position to thoroughly investigate how wave
motion is generated in the solar photosphere, which oscillatory modes are most
prevalent, and the role that these waves play in supplying energy to various
layers of the solar atmosphere.
