Realistic ISM fluctuations from TIGRESS-NCR MHD simulations drive stellar radial heating with σ_R ∝ t^{1/2} (early, cold) and t^{1/5} (late, warm) plus substantial migration explained by quasilinear theory with λ_* ~600 pc and τ_* ~70 Myr.
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FIRE-2 simulations show that stellar radial redistribution scatter saturates at ~2 kpc for stars older than ~3 Gyr, with net orbital changes depending on age and current radius, broadly matching Milky Way observations.
Observational study finds spiral structure correlates with steeper metallicity gradients, larger bulges with shallower gradients and higher metallicities, but no gradient differences from bars or spiral winding tightness.
citing papers explorer
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Interstellar Medium-Driven Orbital Transport -- I. Radial Heating and Migration
Realistic ISM fluctuations from TIGRESS-NCR MHD simulations drive stellar radial heating with σ_R ∝ t^{1/2} (early, cold) and t^{1/5} (late, warm) plus substantial migration explained by quasilinear theory with λ_* ~600 pc and τ_* ~70 Myr.
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Radial redistribution of stellar orbits in FIRE simulations of Milky-Way-mass galaxies
FIRE-2 simulations show that stellar radial redistribution scatter saturates at ~2 kpc for stars older than ~3 Gyr, with net orbital changes depending on age and current radius, broadly matching Milky Way observations.
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The Impact of Bars, Spirals and Bulge-Size on Gas-Phase Metallicity Gradients in MaNGA Galaxies
Observational study finds spiral structure correlates with steeper metallicity gradients, larger bulges with shallower gradients and higher metallicities, but no gradient differences from bars or spiral winding tightness.