Phase-space mixing and the merging of cusps

Details Phase-space mixing and the merging of cusps Phase-space mixing and the merging of cusps

2005-04-11

arxiv.org/abs/astro-ph/0504246v1

Mon.Not.Roy.Astron.Soc. 360 (2005) 869-891

Astronomy and Astrophysics

Astrophysics

9 pages, 5 figures (Fig1 at somewhat lower resolution), accepted for publication in MNRAS

Scientific paper

10.1111/j.1365-2966.2005.09099.x

Collisionless stellar systems are driven towards equilibrium by mixing of phase-space elements. I show that the excess-mass function D(f)= int_{F(x,v)>f} (F(x,v)-f) d^3x d^3v (with F(x,v) the coarse-grained distribution function) always decreases on mixing. D(f) gives the excess mass from values of F(x,v))>f. This novel form of the mixing theorem extends the maximum phase-space density argument to all values of f. The excess-mass function can be computed from N-body simulations and is additive: the excess mass of a combination of non-overlapping systems is the sum of their individual D(f). I propose a novel interpretation for the coarse-grained distribution function, which avoids conceptual problems with the mixing theorem. As an example application, I show that for self-gravitating cusps (rho propto r^{-gamma} as r->0) the excess mass D propto f^{-2(3-gamma)/(6-gamma)} as f->oo, i.e. steeper cusps are less mixed than shallower ones, independent of the shape of surfaces of constant density or details of the distribution function (e.g. anisotropy). This property, together with the additivity of D(f) and the mixing theorem, implies that a merger remnant cannot have a cusp steeper than the steepest of its progenitors. Furthermore, I argue that the remnant's cusp should not be shallower either, implying that the steepest cusp always survives.

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