Signatures of resonance and phase mixing in the Galactic disc. (arXiv:1904.10968v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Hunt_J/0/1/0/all/0/1">Jason A. S. Hunt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bub_M/0/1/0/all/0/1">Mathew W. Bub</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bovy_J/0/1/0/all/0/1">Jo Bovy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mackereth_J/0/1/0/all/0/1">J. Ted Mackereth</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Trick_W/0/1/0/all/0/1">Wilma H. Trick</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kawata_D/0/1/0/all/0/1">Daisuke Kawata</a>
Gaia DR2 has provided an unprecedented wealth of information about the
kinematics of stars in the Solar neighbourhood, and has highlighted the degree
of features in the Galactic disc. We confront the data with a range of bar and
spiral models in both action-angle space, and the $R_{mathrm{G}}-v_{phi}$
plane. We find that the phase mixing induced by transient spiral structure
creates ridges and arches in the local kinematics which are consistent with the
Gaia data. We are able to produce a qualitatively good match to the data when
combined with a bar with a variety of pattern speeds, and show that it is non
trivial to decouple the effects of the bar and the spiral structure.
Gaia DR2 has provided an unprecedented wealth of information about the
kinematics of stars in the Solar neighbourhood, and has highlighted the degree
of features in the Galactic disc. We confront the data with a range of bar and
spiral models in both action-angle space, and the $R_{mathrm{G}}-v_{phi}$
plane. We find that the phase mixing induced by transient spiral structure
creates ridges and arches in the local kinematics which are consistent with the
Gaia data. We are able to produce a qualitatively good match to the data when
combined with a bar with a variety of pattern speeds, and show that it is non
trivial to decouple the effects of the bar and the spiral structure.
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