Authors: Cole Tamburri (CU Boulder, LASP, NSO), Maria Kazachenko (CU Boulder, LASP, NSO), Ryan French (LASP), Adam Kowalski (CU Boulder, LASP, NSO), Rahul Yadav (LASP, NSO), Marcel Corchado-Albelo (CU Boulder, LASP, NSO), Graham Kerr (University of Glasgow), Jiong Qiu (Montana State University), Sarah Riley (Montana State University)

We present impulsive phase observations of a GOES C4.7-class solar flare on 11 August 2024 from the Daniel K. Inouye Solar Telescope. These include Ca II H, Hε, and Hβ spectra from the Visible Spectropolarimeter (ViSP) and Hα images from the Visible Broadband Imager (VBI). Aided by an unsupervised machine learning technique used to cluster ViSP spectra, we analyze the spectrotemporal evolution of individual flare kernels. This analysis reveals significant spatial variability in the spectral behavior of ViSP data, notably four main spectral types: (i) redshifted spectral lines of 20-30 km/s, (ii) unshifted, symmetric line profiles, (iii) spectral lines with central reversals, and (iv) blueshifted spectra of 5-10 km/s. VBI Hα images and ViSP Ca II H intensity maps reveal that the flare ribbon is composed of fragments initially as small as 100-300 km wide that splinter into smaller structures that eventually measure 40-60 km wide. Power spectra of the Hα ribbon intensity suggest that the spatial scales of flare fine structure may be influenced by both pre-flare chromospheric dynamics and flare-time energetics. ViSP spectroscopy demonstrates that the ribbon fragments are characterized by slight elevations in the red wing of Ca II H, indicating that the smallest observed features are formed by downflowing material along coronal loops. For the first time, these flare observations bridge the gap between two recently discovered spatial regimes of solar flare fine structure while simultaneously demonstrating the remarkable spectral diversity present at the smallest observable scales.