Keeping it Cool: Much Orbit Migration, yet Little Heating, in the Galactic Disk

A star in the Milky Way's disk can now be at a Galactocentric radius quite distant from its birth radius for two reasons: either its orbit has become eccentric through radial heating, which increases its radial action $J_R$ (`blurring'); or merely its angular momentum $L_z$ has changed and thereby its guiding radius (`churning'). We know that radial orbit migration is strong in the Galactic low-$α$ disk and set out to quantify the relative importance of these two effects, by devising and applying a parameterized model for the distribution $p(L_z, J_R, τ, \mathrm[Fe/H])$ in the stellar disk. This model describes the orbit evolution for stars of age $τ$ and metallicity [Fe/H], presuming coeval stars were initially born on (near-)circular orbits, and with a unique [Fe/H] at a given birth angular momentum and age. We fit this model to APOGEE red clump stars, accounting for the complex selection function of the survey. The best fit model implies changes of angular momentum of $\sqrt{\langle ΔL_z \rangle^2} \approx 619\, \mathrm{kpc~km/s~}(τ/\mathrm{6~Gyr})^{0.5}$, and changes of radial action as $\sqrt{\langle ΔJ_R \rangle^2} \approx 63\, \mathrm{kpc~km/s~} (τ/\mathrm{6~Gyr})^{0.6}$ at 8 kpc. This suggests that the secular orbit evolution of the disk is dominated by diffusion in angular momentum, with radial heating being an order of magnitude lower.

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