Black Hole (BH)  Introduction to BH  Motivation to study BH  Formation of BH  Cool slides  Size of BH  Properties of BH  Evidence for BH

 Definition of BH  Motivation to study BH  Fascinating ideas (spacetime curvature, event horizon, worm hole etc)  Astronomical observations (quasar, pulsar, AGN, GRB etc)  Quantum Gravity  Astrophysics & High energy particles

Formation of BH  White Dwarf, Pauli Exclusion, electron degeneracy  Temperature >100,000 K  Density  Earth size White Dwarf - 1E9 kg/m 3  Earth - 5.4E3 kg/m 3  Chandrashekar limit 1.4 Solar Mass  Supernova Explosion (>10 Solar Mass)  Neutron star, neutron degeneracy and pulsar  Black Hole and quasar

An Artist's conception of the evolution of our sun through the red giant stage and onto a white dwarf

Birth of a Neutron Star

Supernova explosion -Cas A as seen by the Chandra X- ray Observatory

Vela Pulsar Reveals a Compact Nebula Created by a Shooting Neutron Star

More Red Quasars May Loom in the Universe

Simulation of Black Hole

Black hole in galaxy M87, image from Hubble Space Telescope.

Size of BH - Schwarzschild Radius G=Gravitational Constant For the sun,

Properties of BH  Space time curvature  Compactness and warpage of spacetime  Red shift of light  Event Horizon  boundary of no return  Tidal forces  Singularities  1965 Roger Penrose  Static Black Hole, white hole and worm hole  Naked Singularity  cosmic censorship law  Image frozen in time  Black Hole laws  Black Holes have no hair  Area of Event Horizon and entropy  Hawking Radiation, loss of information, Conservation law of Baryon number

Evidence for BH  Binary Systems Normal star and a BH BH around BH  Active Galactic Nucleus  What are we observing when we are looking for a BH?