Density cusps: restrictions on non-axisymmetric models

Details Density cusps: restrictions on non-axisymmetric models Density cusps: restrictions on non-axisymmetric models

1997-06-17

arxiv.org/abs/astro-ph/9706170v2

Astronomy and Astrophysics

Astrophysics

Corrected some minor typos in equations. 8 pages, tex, with figures, submitted to MNRAS, also at http://www.mpa-garching.mpg.d

Scientific paper

10.1046/j.1365-8711.1998.01413.x

Galactic nuclei are now generally thought to have density cusps in their centres, and the evidence is mounting that as a consequence they are unlikely to be triaxial. Self-consistent stellar dynamical models of non-axisymmetric cusps would be an interesting counter-argument to this conclusion. We consider 2-d analogues of triaxial cusps: a sequence of non-axisymmetric, cuspy discs first described by Sridhar & Touma (1997). Scale-free models with potential {}$\Phi\propto r^\alpha$ are examined in detail. It is shown analytically for $0<\alpha \la 0.43$ that self-consistent models with positive phase-space density do not exist. Numerical solutions of the combined Vlasov and Poisson equations suggest that the whole sequence of models with $0<\alpha<1$ are also unphysical. Along with existing work on cusps, we conclude on purely theoretical grounds that galactic nuclei are not expected to be triaxial.

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