  We present the results of an intensive multi-epoch radio frequency campaign
on the energetic and nearby GRB 171010A with the Karl G. Janksy Very Large
Array and Arcminute Microkelvin Imager Large Array. We began observing GRB
171010A a day after its initial detection, and were able to monitor the
temporal and spectral evolution of the source over the following weeks. The
spectra and their evolution are compared to the canonical theories for
broadband GRB afterglows, with which we find a general agreement. There are,
however, a number of features that are challenging to explain with a simple
forward shock model, and we discuss possible reasons for these discrepancies.
This includes the consideration of the existence of a reverse shock component,
potential microphysical parameter evolution and the effect of scintillation.
