Low-Velocity Streams in the Solar Neighborhood Caused by the Galactic Bar

Details Low-Velocity Streams in the Solar Neighborhood Caused by the Galactic Bar Low-Velocity Streams in the Solar Neighborhood Caused by the Galactic Bar

2009-09-18

arxiv.org/abs/0909.3516v2

Astronomy and Astrophysics

Astrophysics

Galaxy Astrophysics

9 pages, 8 figures, Accepted for publication in MNRAS with minor revisions

Scientific paper

We find that a steady state bar induces transient features at low velocities in the solar neighborhood velocity distribution due to the initial response of the disc, following the formation of the bar. We associate these velocity streams with two quasi-periodic orbital families, librating around the stable x_1(1) and x_1(2) orbits near the bar's outer Lindblad resonance (OLR). In a reference frame moving with the bar, these otherwise stationary orbits precess on a timescale dependent on the strength of the bar, consistent with predictions from a simple Hamiltonian model for the resonance. This behavior allows the two orbital families to reach the solar neighborhood and manifest themselves as clumps in the u-v plane moving away from (x_1(2)), and toward (x_1(1)) the Galactic center. Depending on the bar parameters and time since its formation, this model is consistent with the Pleiades and Coma Berenices, or Pleiades and Sirius moving groups seen in the Hipparcos stellar velocity distribution, if the Milky Way bar angle is 30

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