|
First Stars III
Contact:
|
Talk
Title: The hydrodynamics of galaxy and MBH formation: z < 3 Presenter: Stirling Colgate and Nathan Currier, T-6 Abstract: Most of the baryonic matter, BM, of the current universe is organized into thin, flat rotation curve galaxies with a MBH near their exact center. This requires Òself-organizationÓ on a massive scale. Universally it is agreed that this is initiated by a dark matter, DM, NFW gravitational potential from DM mergers. We claim that the radius of the boundary of this mass is determined by a depletion wave of DM, resulting in the mean galaxy spacing dimension in a Hubble time. Hydrodynamics of the baryonic fraction is initiated at the surprisingly small Reynolds number, Re, ~ 100, and hence very rapid damping of collision-induced turbulence. This allows self-organization of angular momentum, uniformity of density, and uniformity of rotation to take place on integral scales despite many cloud mergers. When mergers are depleted, cooling allows rapid collapse. Rapid collapse allows local conservation of differential rotation because of greatly increased Re and short time. This forms a flat rotation curve, FRC, gaseous mass distribution, M~r, from which a galaxy and MBH form. In these circumstances the primary transport of angular momentum is by 2-D self-gravity and Rossby waves. An inner, 10^5 Msolar central star forms at the radiation trapping radius in the collapse to a FRC where the mass thickness ~ 1/r. The central BH is initiated by accretion onto the remnant neutron star formed by a type II supernova, formed at the center of the 10^5 Msolar central star by pair neutrino emission. The SN disrupts the star and a new one forms by accretion driven by 2-D self-gravity and Rossby waves.
|
