# Caustic rings of dark matter

@inproceedings{Sikivie1997CausticRO,
title={Caustic rings of dark matter},
author={P. Sikivie},
year={1997}
}
88 Citations

## Figures from this paper

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Annals of the New York Academy of Sciences
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In a recent study of 32 extended and well-measured galactic rotation curves, evidence for the self-similar model of galactic halo formation predicts that the caustic ring radii a(n) follow the approximate law a( n) approximately 1/n.
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It has been found that the phase space of dark matter particles assembling a galactic halo in cosmological N-body simulations well defines the fine grained structure. Recently accreted particles form
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. Infall of cold dark matter on a galaxy may result in caustic rings where the particle density is enhanced. They may be searched for as features in the galactic rotation curves. Previous studies
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Caustic rings of dark matter were predicted to exist in the plane of the Galaxy at radii a n ≃ 40 kpc /n for n = 1, 2, 3,.... The recently discovered Monoceros Ring of stars is located near the n = 2
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Limits are placed on the density of any local flow of axions as a function of the flow velocity dispersion over the axion mass range 1.98 to 2.17 microeV.
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Caustic rings of dark matter with $\textit{tricusp}$ cross-section were predicted to lie in the galactic disk. Their radii increase on cosmological time scales at a rate of order $1$ kpc/Gyr. When a
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Although a simple argument implies that the distribution of dark matter in galactic halos is characterized by discrete flows and caustics, their presence is often ignored in discussions of galactic

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