The effects of radial migration on the vertical structure of Galactic discs

We present evidence that isolated growing discs, subject to internal spiral perturbations, thicken due to both heating and radial migration. We show this by demonstrating that the thickness and vertical velocity dispersions of coeval stars depend on their age as well as the change in their radii. Wh...

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Bibliographic Details
Published inMonthly notices of the Royal Astronomical Society Vol. 433; no. 2; pp. 976 - 985
Main Authors Roškar, Rok, Debattista, Victor P., Loebman, Sarah R.
Format Journal Article
LanguageEnglish
Published London Oxford University Press 01.08.2013
Subjects
Accretion disks
Milky Way
Star & galaxy formation
Velocity
Galaxy: evolution
Galaxy: disc
galaxies: kinematics and dynamics
galaxies: evolution
galaxies: spiral
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Summary:We present evidence that isolated growing discs, subject to internal spiral perturbations, thicken due to both heating and radial migration. We show this by demonstrating that the thickness and vertical velocity dispersions of coeval stars depend on their age as well as the change in their radii. While the disc thickens due to internal processes, we find that this induces only a minor amount of flaring. We further demonstrate the consequences of such thickening on the structural properties of stellar populations and find that they qualitatively agree with recent studies of the Milky Way disc.
Bibliography:SourceType-Scholarly Journals-1
ObjectType-Feature-1
content type line 14
ISSN:0035-8711
1365-2966
DOI:10.1093/mnras/stt788