Speaker
Description
Supernova (SN) explosions are one of the most energetic events in the observable universe.
Given that, they are the best natural laboratories to investigate extreme physical phenomena, that otherwise would not be reproducible on Earth.
During these powerful explosions chemical elements are also produced, that go to enrich the amount of heavy elements in the interstellar medium.
Three-dimensional long-time simulations of core-collapse supernovae (CCSNe) are crucial to better understand the connection between the progenitor star and the supernova remnants.
These studies have been performed using mainly two approaches: (i) a detailed 3D analysis of individual events, e.g. SN 1987A (M\"uller et al. 1991; Orlando et al. 2015, 2020), or (ii) 1D surveys of stars with different masses and initial conditions (Ugliano et al. 2012; Sukhbold et al. 2016; Ertl et al. 2020).
Here, we intend to extend the current 3D models in the fashion of the latter 1D simulations, considering SNe originated by different red super giant (RSG) progenitors with zero-age main-sequence (ZAMS) masses between 12.5M⊙ and 27M⊙.
We first study two stars with MZAMS=19.8M⊙ and MZAMS=25.5M⊙.
The first one shows an approximate spherical symmetry in the first stages of the explosion, and asymmetries start to rise only later on.
An interesting case is instead the second model: it shows a peculiar evolution, where the explosion mainly develops on one plane, and it is starting to present structures that recall supernova remnant Cassiopeia A.
This case surely requires further investigation, but having this kind of formations so early in the evolution is really promising.
CCSN simulations are a precious resource for investigating explosion mechanisms and features of the ejecta distribution.
Moreover, from the computational results it is possible to infer some observational properties that can be used to characterize a physical source and retrieve information on its progenitor star.
