1999/06/02 by William H. Kinney, P. Sikivie, Pierre Sikivie · 28 citations
Mathematics · Physics and Astronomy · #Astrophysics #Cosmology and Gravitation Theories #Dark Matter and Cosmic Phenomena #Dark matter #Dark matter halo #Galactic halo #Galaxies: Formation, Evolution, Phenomena #Galaxy #Galaxy rotation curve #Geometry #Halo #Mathematics #Physics #Rotation (mathematics) #astro-ph
paper · pdf · doi:10.1103/physrevd.61.087305
published in Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields 61(8) (American Physical Society) · 4 pages, LaTeX, 1 epsf figure
arxiv created 1999/06/02 · openalex publication_date 2000/03/16 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
The late infall of dark matter onto a galaxy produces structure (such as caustics) in the distribution of dark matter in the halo. We argue that such structure is likely to occur generically on length scales proportional to l\ensuremath∼t0vrot, where t0 is the age of the universe and vrot is the rotation velocity of the galaxy. A set of 32 extended galactic rotation curves is analyzed. For each curve, the radial coordinate is rescaled according to \stackrel\ensuremath→r\stackrel\ifmmode \else \~\fir\ensuremath≡r(v0/vrot), where we choose v0=220 km/s. A linear fit to each rescaled rotation curve is subtracted, and the residuals are binned and averaged. The sample shows significant features near \stackrel\ifmmode \else \~\fir=40 kpc and \stackrel\ifmmode \else \~\fir=20 kpc. This is consistent with the predictions of the self-similar caustic ring model of galactic halos.