  Magnetic bright points on the solar photosphere mark the footpoints of
kilogauss magnetic flux tubes extending toward the corona. Convective buffeting
of these tubes is believed to excite magnetohydrodynamic waves, which can
propagate to the corona and there deposit heat. Measuring wave excitation via
bright-point motion can thus constrain coronal and heliospheric models, and
this has been done extensively with centroid tracking, which can estimate
kink-mode wave excitation. DKIST is the first telescope to provide
well-resolved observations of bright points, allowing shape and size
measurements to probe the excitation of other wave modes that have been
difficult, if not impossible, to study to date. In this work, we demonstrate a
method of automatic bright-point tracking that robustly identifies the shapes
of bright points, and we develop a technique for interpreting measured
bright-point shape changes as the driving of a range of thin-tube wave modes.
We demonstrate these techniques on a MURaM simulation of DKIST-like resolution.
These initial results suggest that modes other than the long-studied kink mode
could increase the total available energy budget for wave-heating by 50%.
Pending observational verification as well as modeling of the propagation and
dissipation of these additional wave modes, this could represent a significant
increase in the potency of wave-turbulence heating models.
