polyrot computes the structure of rotating polytropic bodies. The code computes the equilibrium structure of rotating planets and stars modeled as "polytropes" with pressure and density, and can also compute models including rotation specified as a function of cylindrical radius. polyrot includes a basic plotting function that can show a cross-section along the rotation axis with the colormap indicating density, and a line plotting the surface radius of the star; these and other quantities are attached as attributes to the model.

binary_precursor models light curves of supernova (SN) precursors powered by a pre-SN outburst accompanying accretion onto a compact object companion. Though it is only one of the possible models, it is useful for interpretations of (bright) SN precursors highly exceeding the Eddington limit of massive stars, which are observed in a fraction of SNe with dense circumstellar matter (CSM) around the progenitor. It offers a number of editable parameters, including compact object mass, progenitor mass, progenitor radii, and opacity. Initial CSM velocity can be normalized by the progenitor escape velocity (xi parameter), and the CSM mass, ionization temperature, and binary separation can also be specified.