**Morphological Classification of the Convective Regimes in Rotating Stars** This repository provides movie sequences that support the work appearing in Hindman, Featherstone & Julien (2020), which is currently submitted to the Astrophysical Journal. This work explores the nature and structure of convection in rotating spherical shells that model the interior convection zones of stars. Each numerical model is stored in a separate folder using its model number as a unique label. This model number is the same as that used in Hindman et al. (2020). In addition, the name of the folder indicates the convective regime within which the simulation resides. Within each folder contains one or more movies and two text files. One text file contains the parameters used to generate the numerical model and the other, named 'main_input', is a file used by the simulation code Rayleigh to initialize a run. The movie files are labeled by the name of the physical variable that is animated. Additionally, the name of each movie file contains a code used by the authors to identify a subset of parameters used in the simulations. for example, n3 indicates that three scale heights span the spherical shell; r6 indicates that the star rotates at 6 times the Sun's sidereal Carrington rate; and k2 indicates that the thermal diffusivity is 2 in units of 10$^{12}$ cm$^2$ s$^{-1}$. Each movie shows a field variable on a spherical surface extracted from the full 3D simulations near the outer boundary of the spherical shell. Each movie shows two separate visual vantage points of the same simulation. In the left-hand panel, the viewpoint of the observer is taken just about the equatorial plane, while in the right-hand panel, the observer is looking down from above the north pole. Each vantage point is comoving with the rotating frame of reference. Hence, apparent rotation in these movies is rotation beyond that of the rotating frame.