Velocity peaks and caustic rings

Abstract

The late infall of cold dark matter onto an isolated galaxy produces flows with definite local velocity vectors throughout the galactic halo. It also produces caustic rings, which are places in the halo where the dark matter density is very large. The self-similar model of halo formation predicts that the caustic ring radii $a_n$ follow the approximate law $a_n\simeq 1/n$. I interpret bumps in the rotation curves of NGC 3198 and of our own galaxy as due to caustic rings of dark matter. In this model of our halo the annual modulation effect in direct searches for WIMPs has the opposite sign from that predicted by the isothermal sphere model.

8 pages, 1 figure, to appear in the Proceedings of the 2d International Workshop on the Identification of Dark Matter, Buxton, England, Sept. 7-11, 1998

References in corpus (2)

• Results from a High-Sensitivity Search for Cosmic Axions
• Caustic rings of dark matter

Cited by in corpus (8)

• WIMP Annual Modulation with Opposite Phase in Late-Infall Halo Models
• Velocity distributions and annual-modulation signatures of weakly-interacting massive particles
• Directional recoil rates for WIMP direct detection
• A potential WIMP signature for the caustic ring halo model
• On the direct detection of extragalactic WIMPs
• Gravitational focusing effects on streaming dark matter as a new detection concept
• Axion Structure Formation I: The Co-motion Picture
• DALI sensitivity to streaming axion dark matter