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Accueil > Séminaires > Quantifying radial mixing in disk (…)

Quantifying radial mixing in disk galaxies due to bars

Patricia Sánchez-Blázquez

Numerical simulations have shown that strong gravitational torque by non-axisymmetric components — in particular
bars— induce evolutionary processes such as redistribution of mass and angular momentum in the galactic disks and a consequent change of chemical abundance profiles. The redistribution of stellar disk material influences the interpretation of various critical observed metrics of Galaxy evolution, including the age-metallicity relation in the solar neighborhood and the local G-dwarf metallicity distribution.
However, despite an increased number of theoretical works agree about the importance of
stellar radial migrations for shaping disk galaxies - it is found that > 50% of stars on mostly circular orbits in
the solar neighborhood have come from elsewhere — there is
still a lack of observational evidence probing or quantifying the importance of this process.
I will present star formation histories and the stellar metallicity
gradients in the disk of a sample of nearby galaxies from the Calar
Alto Legacy Integral Field Area Survey (CALIFA).
By comparing these gradients in galaxies with and without bars we
aim to quantify the redistribution of mass and angular momentum in the
galactic disks due to bars