Transcript Black Hole

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/m3
Earth
- 5.4E3 kg/m3
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,
Rs  2  6.7  10
11
30
8 2
 2  10 /(3  10 )  3km
Rs  2GM / c
2
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?