The Boltzmann Moment Equation Approach for the Dynamics of Galactic Stellar Disks

Details The Boltzmann Moment Equation Approach for the Dynamics of Galactic Stellar Disks The Boltzmann Moment Equation Approach for the Dynamics of Galactic Stellar Disks

Aug 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007jena.confe..59v&link_type=abstract

"JENAM-2007, "Our non-stable Universe", held 20-25 August 2007 in Yerevan, Armenia. Abstract book, p. 59-59"

Physics

Scientific paper

I present the BEADS (Boltzmann Equation Approach for the Dynamics of Stars) code that is designed to numerically study the dynamics of galactic stellar disks. The BEADS code solves the Boltzmann moment equations up to second order on a polar grid. The Boltzmann moment equations are closed by the zero-heat-flux approximation. The BEADS-2D code directly evolves observable quantities such as stellar density, mean stellar velocities, and stellar velocity dispersions, which makes it advantageous over more common N-body codes. The BEADS code shows an excellent agreement with the predictions of linear stability analysis for flat stellar disks. The BEADS code is applied to study the influence of spiral structure on the shape and orientation of stellar velocity ellipsoids (SVEs) within the plane of disk galaxies. It is shown that the ratio of the smallest versus largest principal axes of the SVE can take abnormally low values near the outer (convex) edges of stellar spiral arms. The non-axisymmetric gravitational field of a spiral galaxy generates large-scale streams of stars which, in turn, cause considerable vertex deviations in specific regions of the disk. The epicycle approximation is severely broken near the outer edges of spiral arms. These peculiar properties of the SVEs can potentially be used to track the position of stellar spiral arms.

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