Dynamical Models for Disk Galaxies with Triaxial Halos

Abstract

We construct self-consistent dynamical models for disk galaxies with triaxial, cuspy halos. We begin with an equilibrium, axisymmetric, disk-bulge-halo system and apply an artificial acceleration to the halo particles. By design, this acceleration conserves energy and thereby preserving the system's differential energy distribution even as its phase space distribution function is altered. The halo becomes triaxial but its spherically-averaged density profile remains largely unchanged. The final system is in equilibrium, to a very good approximation, so long as the halo's shape changes adiabatically. The disk and bulge are ``live'' while the halo is being deformed; they respond to the changing gravitational potential but also influence the deformation of the halo. We test the hypothesis that halo triaxiality can explain the rotation curves of low surface brightness galaxies by modelling the galaxy F568-3.

23 pages including 9 figures

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Cited by in corpus (11)

• The Core-Cusp Problem
• The Sagittarius Dwarf Galaxy: a Model for Evolution in a Triaxial Milky Way Halo
• Bar formation and evolution in disc galaxies with gas and a triaxial halo: Morphology, bar strength and halo properties
• Cosmology: small scale issues revisited
• The DiskMass Survey. IV. The Dark-Matter-Dominated Galaxy UGC 463
• Dark matter in galaxies
• Loss of halo triaxiality due to bar formation
• Tidal Torquing of Elliptical Galaxies in Cluster Environments
• Interaction between collisionless galactic discs and nonaxissymmetric dark matter haloes
• Order and chaos in a new 3D dynamical model describing motion in non axially symmetric galaxies
• Made-To-Measure Models of Self-Similar Triaxial Halos with Steep Inner Density Gradients