Galaxies are embedded within massive dark matter haloes. The shape of these haloes is expected to be non-spherical (generally triaxial), as suggested by cosmological N-body simulations. The asymmetric gravitational potential influences the dynamics of the disk, which in turn affects the halo itself. With numerical simulations, we can study the role of bar formation in this interplay. By carrying out several high-resolution hydrodynamical simulations using Gadget-2, we are also able to consider the effects of gas in the disc. We find that discs with strong bars contribute to circularize their initially triaxial haloes.
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- Machado R E G, Athanassoula E. Loss of halo triaxiality due to bar formation. MNRAS, 2010, 406, 2386.