The origin of cores and density profiles of gaseous baryonic structures

Abstract

We study the origin of cores and density profiles of gaseous baryonic structures in cosmology. By treating the baryons as a viscous gas, we find that both spheres and disks are possible solutions. We find analytically that the density profiles have inner and outer solutions, which in general are different. For disks we identify a central core, with density profile rho_d = constant, and the outer profile rho_d ~ r^{-3}. For spherical structures we find the profile rho_s ~ r^{-6}. In the presence of a dominating central black hole we find the inner profile rho ~ r^{-3/2}. When the mass is dominated by a dark matter component then the baryonic density profile will depend on the dark matter profile, and we point out how one can use this connection to infer the DM profile directly by observing the baryonic density profile.

arXiv comment6 pages, 2 figures, new introduction, improved discussion, conclusions unchanged (as accepted in apjl)

References in corpus (8)

• The Structure of Cold Dark Matter Halos
• Cold collapse and the core catastrophe
• Dark matter and visible baryons in M33
• Chandra Observations of Abell 2029: The Dark Matter Profile Down to <0.01 R_vir in an Unusually Relaxed Cluster
• A new Monte Carlo code for star cluster simulations: II. Central black hole and stellar collisions
• Direct Detection of Dark Matter in Supersymmetric Models
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Cited by in corpus (8)

• Cluster Heating by Viscous Dissipation of Sound Waves
• 3D simulations of viscous dissipation in the intracluster medium
• Dark matter density profiles from the Jeans equation
• Standing and travelling waves in the shallow-water circular hydraulic jump
• Dynamical signatures of infall around galaxy clusters: a generalized Jeans equation
• Cluster temperature profiles and Sunyaev-Zeldovich observations
• The density profiles of hot galactic halo gas
• Dissipation and acoustic tunnelling about the sonic horizon of Bondi accretion