Abstract
A strong bar rotating within a massive halo should lose angular momentum to the halo through dynamical friction, as predicted by Weinberg. We have conducted fully self-consistent, numerical simulations of barred galaxy models with a live halo population and find that bars are indeed braked very rapidly. Specifically, we find that the bar slows sufficiently within a few rotation periods that the distance from the centre to co-rotation is more than twice the semi-major axis of the bar. Observational evidence (meagre) for bar pattern speeds seems to suggest that this ratio typically lies between 1.2 to 1.5 in real galaxies. We consider a number of possible explanations for this discrepancy between theoretical prediction and observation, and conclude that no conventional alternative seems able to account for it.
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© 1996 Springer-Verlag P203 0201 V 2
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Sellwood, J.A., Debattista, V.P. (1996). Secular evolution in barred galaxies. In: Sandqvist, A., Lindblad, P.O. (eds) Barred Galaxies and Circumnuclear Activity. Lecture Notes in Physics, vol 474. Springer, Berlin, Heidelberg. https://doi.org/10.1007/BFb0101964
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DOI: https://doi.org/10.1007/BFb0101964
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