Estudios numéricos de supernovas

The evolution of massive stars constitutes a very active field of astrophysics. There are important implications for the ends of these stars as supernovae explosions, where compact objects are formed, and the surrounding interstellar medium is mobilized and enriched. The first data can help understand the environment where the explosion occurs. This is why recent decades have seen to flourish the observational efforts to discover supernovae, allowing them to be detected at increasingly earlier times. The number of studies and detections in different bands, beyond the visual range, has also grown, and it has been proposed to identify new types of transients. The study of peculiar cases thus becomes relevant: recent findings include, for example, new cases of supernovae with two maxima in the evolution of brightness following a morphology that may challenge the most accepted scenario. In this talk we will recognize the contributions that are made from hydrodynamic modeling techniques, both for now better characterized populations, and for some of the supernovae that deviate from the conventional. The results that I will show arise from calculating in a one-dimensional way the propagation of the shock wave in the interior and upper stellar layers, added to the energy contribution of the decay of radioactive elements, or eventually the presence of a central object, which can provide an important contribution of additional energy.