Rapid (r) neutron capture process yields are fundamental for precise modeling and interpretation of kilonova (KN) spectra, and are determined via nuclear reaction network calculations or inferred from the slow (s) neutron capture yields. We intend to create an open-source Python software package for managing and analyzing s & r process theoretical abundances derived from nuclear network calculations and spectroscopic observations. We also will develop a user-friendly web interface for streamlined access to s & r process yields from public databases. Our pilot project aims to enhance community access to pivotal data for KN modeling and the study of the Universe chemical evolution. Over time, this tool will be extended to opacity tables, as well as KN theoretical light curves and spectra.
Interacting binary systems are the progenitors of many eruptive phenomena determined by the transfer of mass onto degenerate compact object (white dwarfs). Among the other we recall Type Ia Supernovae, which are one of the main contributor to the galactic iron and which can be used as standardized distance indicators to probe the far Universe and, hence, to characterize the equation of state of the dark energy component. However, the currently understanding of the evolution of binary systems is far to be complete and satisfactory, as a self-consistent treatment of the mass transfer process is still missing. For this reason the proposed project aims to develop a new numerical tool able to model the evolution of both the two components in interacting binaries, by accounting for the modification of the binary parameters as determined by the mass transfer process.