Completed
BH: evidence for supermassive black holes log nM Black Hole Mass Distribution
Class Central Classrooms beta
YouTube videos curated by Class Central.
Classroom Contents
Formation, Fueling, and Feedback from Supermassive Black Holes - Lecture 1
Automatically move to the next video in the Classroom when playback concludes
- 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