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

By R. Rovskar, V. Debattista, Sarah Loebman. 2012

67 citations recorded by the source corpus.

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.

Subfields: Astronomy and Astrophysics

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Citations in the corpus

Yule-Simpson’s paradox in Galactic Archaeology (2019, background): “…larger radii are kinematically hotter than those born at smaller radii is remarkable as it provides, for the first time, observational evidence that outward migration cools the local disk, rather than heat it, as has been proposed in the past (e.g., Schönrich & Binney 2009b; Roškar et al. 2013).”
Constraining the thick disc formation scenario of the Milky Way (2014, unknown): “The flare, which is absent in the main thick disc, agrees well with this scenario, while other scenarios such as radial migration or thin-disc heating by mergers would have produced a significant flare in the outer thick disc (Minchev et al. 2012; Roškar et al. 2013).”
THE EFFECT OF RADIAL MIGRATION ON GALACTIC DISKS (2014, background): “These biases have been hinted at in earlier work (see, e.g., Minchev et al. 2012b; Solway et al. 2012; Bird et al. 2012; Roškar et al. 2013) but their importance has not been properly appreciated, obscured perhaps by the concurrence of other heating mechanisms (i.e., satellite perturbations, disk…”
The age structure of stellar populations in the solar vicinity Clues of a two-phase formation history of the Milky Way disk (2013, background): “Similarly, Roškar et al. (2013) predict that the outer disk should be essentially younger than 2 Gyr following Bovy et al. (2012b).”
Numerical simulation of a possible origin of the positive radial metallicity gradient of the thick disk (2013, background): “Figure 4 shows a “flaring” feature (e.g. Bird et al. 2012, 2013; Roškar et al. 2013) for the younger stars.”
THE RELATIONSHIP BETWEEN MONO-ABUNDANCE AND MONO-AGE STELLAR POPULATIONS IN THE MILKY WAY DISK (2016, methodology): “Formation of thick disks by radial migration was proposed as a mechanism by Schönrich and Binney (2009), later on advocated by Loebman et al. (2011) and Roškar et al. (2013).”
Impacts of a flaring star-forming disc and stellar radial mixing on the vertical metallicity gradient (2016, background): “…vertical metallicity gradient for the thin disc population is not well studied (for studies for the combined populations of thin and thick discs, see e.g. Kobayashi & Nakasato 2011; Loebman et al. 2011; Pilkington et al. 2012; Roškar et al. 2013; Miranda et al. 2016; Schönrich & McMillan 2016).”
Estimating stellar birth radii and the time evolution of Milky Way’s ISM metallicity gradient (2018, background): “The result that stars born at larger radii are kinematically hotter than those born at smaller radii is remarkable as it indicates that outward migration cools the local disk, rather than heat it, as has been proposed in the past (Schönrich & Binney 2009; Roškar et al. 2013).”
TRACING CHEMICAL EVOLUTION OVER THE EXTENT OF THE MILKY WAY'S DISK WITH APOGEE RED CLUMP STARS (2014, background): “While some simulations produce lowmetallicity, low-α stars (e.g., Roškar et al. 2013), they fail to reproduce the observed intermediate-α valley.”
Vertical disc heating in Milky Way-sized galaxies in a cosmological context (2015, background): “• The overall effect of radial migration on the present day vertical disc is sub-dominant for all coeval populations, which suggests that radial migration cannot thicken preexisting stellar distributions (contrary to what is reported by, e.g., Schönrich & Binney 2009; Roškar et al. 2013).”
THE STELLAR POPULATION STRUCTURE OF THE GALACTIC DISK (2015, background): “…that may have occurred in the MW, current simulations do indicate that kinematic biases in the population of migrators are significant enough that little or no effect on the vertical structure of the disk should be expected (Minchev et al. 2012; Roškar et al. 2013; Vera-Ciro et al. 2014).”