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.
year = 1966, month = dec, volume =
3 Pith papers cite this work. Polarity classification is still indexing.
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Clumps in high-redshift spiral galaxies are smaller than commonly reported, spatially concentrated toward spiral arms, smaller but brighter inside arms than between them, with similar colors, suggesting arms stimulate clump formation but do not alter their star formation properties.
A two-wave radial corrugation model fitted to LAMOST and Gaia data reproduces the observed periodic radial velocity variations and explains the inner-outer disk transition in the Milky Way.
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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Clumps in spiral galaxies at $z \lesssim 3$: Disentangling two spatial modes of star formation
Clumps in high-redshift spiral galaxies are smaller than commonly reported, spatially concentrated toward spiral arms, smaller but brighter inside arms than between them, with similar colors, suggesting arms stimulate clump formation but do not alter their star formation properties.
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The multiple corrugations in the Galactic disk derived from the LAMOST and Gaia survey data
A two-wave radial corrugation model fitted to LAMOST and Gaia data reproduces the observed periodic radial velocity variations and explains the inner-outer disk transition in the Milky Way.