Methodological Characterization and Computational Codes in the Simulation of Interacting Galaxies

Abstract

Currently, technological development has exponentially fostered a growing collection of dispersed and diversified information. In the case of galaxy interaction studies, it is important to identify and recognize the parameters in the process, the tools and the computational codes available to select the appropriate one in depending on the availability of data. The objective was to characterize the parameters, techniques and methods developed, as well as the computational codes for numerical simulation. From the bibliography, it was reviewed how various authors have studied the interaction, presence of gas and star formation, then the review of computer codes with the requirements and benefits, to analyze and compare the initial and boundary conditions. With images, the CNN method programmed in python was applied to identify the differences and their possible accuracy. SPH systems have more robust algorithms, invariance, simplicity in implementation, flexible geometries, but do not parameterize artificial viscosities, discontinuous solutions and instabilities. In the case of AMR there is no artificial viscosity, resolution of discontinuities, suppression of instabilities, but with complex implementation, mesh details, resolution problems and they are not scalable. It is necessary to use indirect methods to infer some properties or perform preliminary iterations. The availability of observable data governs the behavior of possible numerical simulations, in addition to having tools such as a supercomputer, generating errors that can be adjusted, compared or verified, according to the techniques and methods shown in this study, in addition to the fact that codes that are not so well known and used stand out as those that are currently more applied.