A review of Gaia-era Milky Way dynamics concludes that the disc is strongly out of equilibrium and that most recent evidence favors a long, slowly rotating bar, while the bar pattern speed and dark halo properties remain unsettled.
The Splash without a merger
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abstract
The Milky Way's progenitor experienced several merger events which left their imprints on the stellar halo, including the Gaia-Sausage/Enceladus. Recently, it has been proposed that this event perturbed the proto-disk and gave rise to a metal rich ([Fe/H] $>-1$) low angular momentum ($v_{\phi} < 100$ km/s) stellar population. These stars have dynamical and chemical properties different from the accreted stellar halo, but are continuous with the canonical thick disk. In this letter, we use a hydrodynamical simulation of an isolated galaxy which develops clumps that produce a bimodal thin$+$thick disk chemistry to explore whether it forms such a population. We demonstrate clump scattering forms a metal-rich, low angular momentum population, without the need for a major merger. We show that, in the simulation, these stars have chemistry, kinematics and density distribution in good agreement with those in the Milky Way.
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Milky Way dynamics in light of Gaia
A review of Gaia-era Milky Way dynamics concludes that the disc is strongly out of equilibrium and that most recent evidence favors a long, slowly rotating bar, while the bar pattern speed and dark halo properties remain unsettled.