2016/06/09 by Nir J. Shaviv, Shaviv, Nir J. · 1 citation
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysics of Galaxies (astro-ph.GA) #FOS: Physical sciences #High Energy Physics - Phenomenology (hep-ph) #Scientific Research and Discoveries #Stellar, planetary, and galactic studies
paper · pdf · doi:10.48550/arxiv.1606.02851
openalex publication_date 2016/06/09 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
Using a recent geochemical reconstruction of the Phanerozoic climate which exhibits a 32 Ma oscillation with a phase and the secondary modulation expected from the vertical the motion of the solar system perpendicular to the galactic plane (shaviv et al. 2014), we show that a kinematically cold strongly interacting disk dark matter (dDM) component is necessarily present in the disk. It has a local density ρdDM = 0.11 ± 0.03 M\odot/pc3. It is also consistent with the observed constraints on the total gravitating mass and the baryonic components, and it is the natural value borne from the Toomre stability criterion. It also has surface density ΣdDM = 15 ± 5 M\odot/pc2 and a vertical velocity dispersion of σW = 8.0 ± 4.5 km/s. A dense ("dinosaur killing") thin disk is ruled out. The "normal" halo dark matter (hDM) component should then have a local density ρhDM \lesssim 0.01 M\odot/pc3. If the dDM component follows the baryons, its average density parameter is ΩdDM = 1.5 ± 0.5% and it comprises about 1/8 to 1/4 of Milky Way (MW) mass within the solar circle.