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Lecture 1: Basics of Black Holes & Accretion
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Formation, Fueling, and Feedback from Supermassive Black Holes - Lecture 1
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- 1 Lecture 1: Basics of Black Holes & Accretion
- 2 Lecture 1: Outline
- 3 Key Physics Challenge of Scales for BHs
- 4 Schwarzschild Solution space-time geometry point mass
- 5 BHs: evidence for stellar mass black holes lognM Black Hole Mass Distribution
- 6 BH: evidence for supermassive black holes log nM Black Hole Mass Distribution
- 7 BH: primordial black holes: not yet ruled out log nM Black Hole Mass Distribution
- 8 Primordial BHs
- 9 What are primordial BHs?
- 10 Why do we care about PBH
- 11 Astrophysical constraints:
- 12 Masses in the Stellar Graveyard
- 13 Observational Evidence for Stellar Mass Black Holes
- 14 Evidence For Elusive Imbhs From An Observed Tidal Disruption Events TDEs
- 15 This is the most efficient known way of using mass to get energy:
- 16 accretion on to a black hole must power the most luminous phenomena in the universe
- 17 Eddington implies limit on growth rate of mass: since
- 18 Emitted spectrum of an accrediting object
- 19 b Gravitational energy of each accreted electron-proton pair turned directly into heat at shock temperature
- 20 For supermassive black holes we have
- 21 Modelling accreting sources
- 22 examine both problems in the following
- 23 Accreting Black Holes in a Nearby Galaxy M1011
- 24 Bondi-Hoyle Lyttleton Accretion
- 25 Accretion disc formation
- 26 Thus in general matter orbits accretor. What happens?
- 27 accretion disc structure see APIA Ch 5
- 28 disc formation is unavoidable
- 29 Accretion discs are universal:
- 30 accretion disc structure
- 31 Q&A
