Dissecting the Phase Space Snail Shell

Abstract

Abstract The ongoing vertical phase-mixing, manifesting itself as a snail shell in the phase space, has been discovered with Gaia DR2 data. To better understand the origin and properties of the phase-mixing process, we study the vertical phase-mixing signatures in arches (including the classical “moving groups”) of the phase space near the solar circle. Interestingly, the phase space snail shell exists only in the arches with km s−1, i.e., stars on dynamically “colder” orbits. The snail shell becomes much weaker and eventually disappears for increasingly larger radial action (J R ), quantifying the “hotness” of orbits. Thus, one should pay closer attention to the colder orbits in future phase-mixing studies. We also confirm that the Hercules stream has two branches (at fast and slow V ϕ ), which may not be explained by a single mechanism, since only the fast branch shows the prominent snail shell feature. The hotter orbits may have phase-wrapped away already due to the much larger dynamical range in radial variation to facilitate faster phase-mixing. To explain the lack of a well-defined snail shell in the hotter orbits, the disk should have been perturbed at least 500 Myr ago. Our results offer more support to the recent satellite-disk encounter scenario than the internal bar-buckling perturbation scenario as the origin of the phase space mixing. The origin of the more prominent snail shell in the V ϕ color-coded phase space is also discussed.