Implications of Stellar Migration for the Properties of Galactic Disks

Details Implications of Stellar Migration for the Properties of Galactic Disks Implications of Stellar Migration for the Properties of Galactic Disks

Jan 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21535404r&link_type=abstract

American Astronomical Society, AAS Meeting #215, #354.04; Bulletin of the American Astronomical Society, Vol. 42, p.537

Astronomy and Astrophysics

Astronomy

Scientific paper

Recent theoretical work suggests that it may be common for stars in the disks of spiral galaxies to migrate radially across significant distances. Such migrations are a result of spiral corotation resonance scattering and move the guiding centers of the stars while preserving the circularities of their orbits.Migration can therefore efficiently mix stars in all parts of the disk. Therefore, if migration does indeed occur in real disks, it requires that disks be thought of as fully inter-connected structures with a common history rather then a set of autonomous regions. In the extreme, radial migration allows the evolution of the innermost regions to contribute significantly to the outermost parts of the disk. I will discuss the results from a suite of idealized N-body/SPH simulations of disk formation and evolution, spanning a range in the parameter space of galaxy properties. I will focus on the insight we can gain from simulations when interpreting observational data of a full range of stellar systems, including the solar neighborhood, the thick and thin disks of the Galaxy, as well as external disks, in particular their outermost regions. I will demonstrate that radial migration needs to be considered in studies of galactic disk evolution, and discuss some of our recent attempts to do so with observational data from SDSS and HST.

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