On the relevance of chaos in the solar neighbourhood IV

N. P. MAFFIONE; F. A. GOMEZ; P. M. CINCOTTA; C. M. GIORDANO

Congreso; 61 Reunión Anual de la Asociación Argentina de Astronomía; 2019

We have been working with realistic samples of the stellar halo component in the neighbourhood of the Sun provided by the Auriga Milky Way (MW) mass-type galaxies (a suite of state-of-the-art fully cosmological magneto--hydrodynamical simulations) and analytical models used to compute chaos indicators. We showed in a previous paper that using a multicomponent time--independent representation of a MW--type galaxy, chaos might be present (20\%) but chaotic diffusion should not be important on erasing local signatures of past galactic accretion events, a result that has been validated so far thanks to the latest observations provided by GAIA. In order to extend our analysis from the local stellar halo to the disk component, we have revisited the analytical model and provide a more realistic representation of the MW. Therefore, herein we present our new multicomponent time--dependent analytical model that is able to account for the impact of the bar and spiral arms and help researchers to study dynamical phenomena on the disk of MW--type galaxies. Some preliminary results on the dynamics of the disk are also presented.