Radial Mixing in the Milky Way Disk Caused by Spiral-Bar Resonance Overlap

Details Radial Mixing in the Milky Way Disk Caused by Spiral-Bar Resonance Overlap Radial Mixing in the Milky Way Disk Caused by Spiral-Bar Resonance Overlap

Jan 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21560701m&link_type=abstract

American Astronomical Society, AAS Meeting #215, #607.01; Bulletin of the American Astronomical Society, Vol. 36, p.1138

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Scientific paper

While it has long been known that a large number of short-lived transient spirals can cause stellar migration, here we report that quasi-stationary spiral structure, or equivalently a small number of long-lived transients, interacting with a central bar is another effective mechanism for radial mixing in galactic disks. Although angular momentum changes are concentrated near the corotation radius of each individual perturber, due to the non-linear coupling between the bar and spirals the entire disk is affected. A large fraction of stars near the solar circle could have originated in the Milky Way outer disk, provided the bar's 2:1 outer Lindblad resonance is close to the 4:1 inner Lindblad resonance of a 4-armed spiral structure. For this choice of parameters, changes in angular momentum occur 3 times faster than in the case of recurrent spirals. As a consequence, mixing in barred galaxies with transient spirals must be much more efficient than in unbarred galaxies. We also find that velocity dispersion increases with time in a manner consistent with observations. This new mechanism could account for both the observed age-velocity relation and the absence of age-metallicity relation in the solar neighborhood. Support for this work was provided by ANR and RAVE.

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