On the relevance of chaos in the solar neighbourhood III

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

La Serena

Congreso; Segunda Reunión Binacional AAA-SOCHIAS 2018; 2018

Universidad de La Serena

In order to locally characterize the impact of chaos in the assembling history of our Milky Way (MW), we havebeen working with a combination of cosmological magneto-hydrodynamical simulations (the Auriga suite) and analytical models. The simulations provide us with realistic samples of the stellar component in solar neighbourhood-like volumes as well as values for the structural parameters of MW{type galaxies. The analytical models are calibrated with such parameter values and used to integrate the initial conditions to compute chaos indicators. In previous works we showed that using a time-independent representation of a MW-type galaxy consisting of a nuclear region with a supermassive black hole, a bulge, an exponential disk and a dark matter halo, chaos might be present (around 20%) but chaotic diffusion should not be important on erasing local signatures of past galactic accretion events. Our theoretical results are currently being validated thanks to the latest observations provided by GAIA. The success of our strategy pushes us to further improve our analytical models. Herein we review previous results and present our new analytical model that accounts for the effects of a bar and spiral arms.