Astronomy and Astrophysics – Astrophysics
Scientific paper
Apr 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aps..aprd11009c&link_type=abstract
American Physical Society, April Meeting, Jointly Sponsored with the High Energy Astrophysics Division (HEAD) of the American As
Astronomy and Astrophysics
Astrophysics
Scientific paper
The central galactic black hole, BH, mass is predicted from the mass and angular momentum, λ_cloud ~= 0.07, prior to collapse of a Lyman-α cloud. Semi-spherical shape, initial uniform rotation, Keperian support, and local conservation of angular momentum, ensures a near flat rotation curve (FRC), M_interior ∝ R as observed. Rapid collapse, ~ 10^7 years before most star formation, leads to a disk, primarily of gas whose mass thickness, Σ_FRC ∝ 1/R. At small radii, R ~ 10 pc, the mass thickness exceeds the condition for the formation of the Rossby vortex instability, (RVI), Σ_FRC ~ 100 g cm-2. The RVI allows angular momentum to be transported, and so the interior mass, M_interior ~= 10^8 M_solar, nearly all collapses as an accretion disk to a BH. Then σ_velocity ∝ M_BH^4. The transport length of a Rossby vortex in an RVI disk is ~ R compared to the height, ~ H in a diffusive, Shakura- Sunyaev disk so that self gravitating excessive disk mass does not occur. A dynamo forms naturally within this disk inside radii, ~ 0.01 pc where the gas becomes ionized and where the helicity is created from star disk collisions. Saturation of the dynamo at the back reaction limit ensures that a significant fraction of the formation energy can be transformed into magnetic energy. A small fraction of this energy, ~ 10-4, deposited outside the disk may form the galactic bulge.
Colgate Stirling
Hui Li
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