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Putting this in the equation for sigma and using the Kepler form of angular velocity we get
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Formation, Fueling, and Feedback from Supermassive Black Holes - Lecture 2
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- 1 Formation, Fueling, and Feedback from Supermassive Black Holes Lecture 2
- 2 accretion disc structure
- 3 Thin Accretion Discs
- 4 Viscosity
- 5 Net torque on disc ring between R, R +
- 6 Remaining term represents dissipation:
- 7 Assume now that disc matter has a small radial velocity VR
- 8 For accretion disc equations etc
- 9 Steady thin discs
- 10 Putting this in the equation for sigma and using the Kepler form of angular velocity we get
- 11 Now if disc optically tick and radiates roughly as a blackbody,
- 12 Condition for a thin disc HR
- 13 Disc timescales
- 14 size of AGN disc set by self gravity
- 15 central object gains a.m. and spins up at rate
- 16 accretion to central object
- 17 motion near a point mass
- 18 motion near a black hole
- 19 where are the holes? dynamical friction
- 20 dynamical friction
- 21 centre of Milky Way
- 22 spinning Kerr black hole
- 23 Eddington limit
- 24 Can a black hole ignore the Eddington limit?
- 25 Super-Eddington Accretion
- 26 cosmological picture of growth: big galaxy swallows small
- 27 galaxy knows about central SMBH
- 28 how?
- 29 well....
- 30 LECTURE 2: OUTLINE
- 31 Accretion Disk Structure & Emergent Spectrum
- 32 Disk Temperature
- 33 Disk Spectrum
- 34 Emission from AGN
- 35 Active Galactic Nuclei AGN
- 36 The Lay of the Land
- 37 AGN spectrum: broad-band + variability
- 38 Accretion Disk Corona & Torus
- 39 Broad & Narrow Absorption-Lines
- 40 Radio Galaxies and Jets
- 41 Jets: Focussed Streams of Ionized Gas
- 42 Thin discs?
- 43 Viscosity
- 44 Black Holes Scaling Relations
- 45 Globally averaged BHAR traces over cosmic time
- 46 Understanding Mbh - sigma
- 47 Q&A
