  It is well known that the dominant frequency of oscillations in the solar
photosphere is $\approx$3 mHz, which is the result of global resonant modes
pertaining to the whole stellar structure. However, analyses of the horizontal
motions of nearly 1 million photospheric magnetic elements spanning the
entirety of solar cycle 24 have revealed an unexpected dominant frequency,
$\approx$5 mHz, a frequency typically synonymous with the chromosphere. Given
the distinctly different physical properties of the magnetic elements examined
in our statistical sample, when compared to largely quiescent solar plasma
where $\approx$3 mHz frequencies are omnipresent, we argue that the dominant
$\approx$5 mHz frequency is not caused by the buffeting of magnetic elements,
but instead is due to the nature of the underlying oscillatory driver itself.
This novel result was obtained by exploiting the unmatched spatial and temporal
coverage of magnetograms acquired by the Helioseismic and Magnetic Imager (HMI)
on board NASA's Solar Dynamics Observatory (SDO). Our findings provide a timely
avenue for future exploration of the magnetic connectivity between
sub-photospheric, photospheric, and chromospheric layers of the Sun's dynamic
atmosphere.
