Radial migration in galactic disks caused by resonance overlap of multiple patterns: Self-consistent simulations

By I. Minchev, B. Famaey, F. Combes, Paola Di Matteo, M. Mouhcine, H. Wozniak. 2010

140 citations recorded by the source corpus.

We have recently identified a new radial migration mechanism resulting from the overlap of spiral and bar resonances in galactic disks. Here we confirm the efficiency of this mechanism in fully self-consistent, Tree-SPH simulations, as well as high-resolution pure N-body simulations. In all barred cases we clearly identify the effect of spiral-bar resonance overlap by measuring a bimodality in the changes of angular momentum in the disk, ΔL, whose maxima are near the bar's corotation and outer Lindblad resonance. This contrasts with the smooth distribution of ΔL for a simulation with no stable bar present, where strong radial migration is induced by multiple spirals. The presence of a disk gaseous component appears to increase the rate of angular momentum exchange by about 20%. The efficiency of this mechanism is such that galactic stellar disks can extend to over 10 scale-lengths within 1-3 Gyr in both Milky Way size and low-mass galaxies (circular velocity ~ 100 km s -1 ). We also show that metallicity gradients can flatten in less than 1 Gyr rendering mixing in barred galaxies an order of magnitude more efficient than previously thought.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/809d38fbf7c4040d9679d9fc3373e5c78121a3fc

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

Citations in the corpus

Constraining the thick disc formation scenario of the Milky Way (2014, unknown): “The importance of migrations has been shown by Sellwood & Binney (2002) and has been studied in different N-body simulations (Roškar et al. (2012); Minchev et al. (2011); Di Matteo et al. (2011); Bird et al. (2012) among others).”
The dynamics of stars around spiral arms (2011, background): “…1985; Amaral & Lepine 1997; Sellwood & Binney 2002; Minchev & Quillen 2006; Roškar et al. 2008a; Roškar et al. 2008b; Sánchez-Blázquez et al. 2009; Minchev et al. 2011) and in barred-spiral galaxies where a bar resonance is also included (e.g. Minchev & Famaey 2010; Manos & Athanassoula 2011).”
THE VERTICAL METALLICITY GRADIENT OF THE MILKY WAY DISK: TRANSITIONS IN [α/Fe] POPULATIONS (2014, background): “…involves stars moving radially from the inner to – 5 – the outer regions of the disk, and vice versa, due to scattering by transient spiral structure (Sellwood & Binney 2002) or diffusion caused by overlap of bar-spiral resonances (Minchev & Famaey 2010; Brunetti et al. 2011; Minchev et al. 2011).”
The effects of radial migration on the vertical structure of Galactic discs (2012, background): “At later times, the phenomenon driving the disc trends in their models (the same simula- c© 0000 RAS, MNRAS000, 000–000 tions were also discussed in Minchev et al. 2011 and Minchev et al. 2012b) is efficient angular momentum redistribution duringbar growth (e.g. Hohl 1971) as opposed to more…”
The Milky Way’s stellar disk (2013, background): “What has been the role of radial migration (Sellwood & Binney 2002; Roškar et al. 2008a,b; Schönrich & Binney 2008; Minchev et al. 2011), i.e., the substantive changes in the stars’ mean orbital radii that are expected to occur without boosting the orbits’ eccentricity?”
Chemodynamical evolution of the Milky Way disk - I. The solar vicinity (2012, background): “However, how exactly radial migration affects disk thickening in dynamical models had not been demonstrated (but only assumed) until the recent work by Minchev et al. (2011b) and Minchev et al. (2012b).”
New constraints on the chemical evolution of the solar neighbourhood and galactic disc(s) - improved astrophysical parameters for the Geneva-Copenhagen Survey (2011, background): “The presence of a bar would rather imply the existence of an old metal-rich population, which we do not detect (but see Minchev & Famaey 2010; Minchev et al. 2011, for a recent dis- cussion on the effect of the bar).”
Radial migration does little for Galactic disc thickening (2012, methodology): “(ii) Flattening of the average vertical action radial profile: As pointed out by Minchev et al. (2011b), an important consequence of the conservation of actions for migrating stars is that radial migration also mixes the radial distributions of the actions 〈Jp〉 and 〈Jz〉: the more the disc mixes,…”
SELF-PERPETUATING SPIRAL ARMS IN DISK GALAXIES (2012, background): “…for a better understanding for how stars like the Sun can migrate if the nature and the evolution of the waves is different (Roškar et al. 2008; Minchev et al. 2011) We anticipate that there should be a correlation between the amplitude of the arms and the Q parameter that defines…”
Radial migration in disc galaxies — I. Transient spiral structure and dynamics (2011, background): “Minchev & Famaey (2010); Minchev et al. (2011, 2012) argued that apart from corotation scattering as presented by SB02, combined effects of multiple nearby resonances from several different patterns may alsobe important in driving the redistribution of stars.”
Constraining the Milky Way assembly history with Galactic Archaeology (2016, methodology): “A number of works using Nbody and N-body/SPH simulations (e.g., Grand et al. 2012; Minchev et al. 2011; Roškar et al. 2008) have confirm that migration always takes place in numerical galactic discs.”
Chemodynamical evolution of the Milky Way disk II: Variations with Galactic radius and height above the disk plane (2014, background): “…of angular momentum has been shown to be caused by the effect of non-axisymmetric disk features, such as spiral structure (Sellwood and Binney, 2002; Roškar et al., 2008) and the central bar (Minchev and Famaey, 2010; Minchev et al., 2011; Brunetti et al., 2011; Di Matteo et al., 2013).”
THE SPATIAL STRUCTURE OF MONO-ABUNDANCE SUB-POPULATIONS OF THE MILKY WAY DISK (2011, background): “…of angular momentum without radially heating the disk (“radial migration”) happens naturally if spiral structure is transient (Sellwood & Binney 2002; Roškar et al. 2008, 2011), and has also been shown to occur through bar–spiral structure interactions (Minchev & Famaey 2010; Minchev et al. 2011).”
Estimating stellar birth radii and the time evolution of Milky Way’s ISM metallicity gradient (2018, background): “…of the inside-out disk formation and the stellar surface density exponential falloff with radius, the metallicity gradient of a mono-age population outside the bulge/bar will always tend to flatten with time due to both radial migration and blurring (Roškar et al. 2008; Minchev et al. 2011).”
Evolution of galactic discs: multiple patterns, radial migration, and disc outskirts (2012, methodology): “1 in Minchev et al. 2011a), the differential densityΣdi f displays strong variations with radius with prominent discontinuities (strong decreas in amplitude) in the spirals.”
THE EFFECT OF RADIAL MIGRATION ON GALACTIC DISKS (2014, background): “…& Helmi 2008; Bird et al. 2012), whereas others have focused on hydrodynamical simulations of disks of gas and stars that evolve in isolation (Minchev et al. 2011, 2012b) or that result from the dissipative collapse of a rotating sphere of gas in the gravitational potential of a dark matter…”
The age structure of stellar populations in the solar vicinity Clues of a two-phase formation history of the Milky Way disk (2013, background): “…been discussed in the literature A109, page 14 of 18 (Sellwood & Binney 2002; Schönrich & Binney 2009a; Roškar et al. 2008; Minchev & Famaey 2010; Minchev et al. 2011, 2012a,b; Di Matteo et al. 2013) is the result of a secular process related to the presence of stellar asymmetries likes bars and…”
The Lives of Stars: Insights from the TGAS–RAVE–LAMOST Data Set (2018, background): “…Famaey (2010) expanded on this with the addition of a bar component and found that bars may affect angular momentum change in the vicinity of the corotation radius and the outer Lindblad resonance and also that bars may enhance the rate at which metallicity gradients flatten (Minchev et al. 2011).”