1. Chapter 22: Black Holes Einstein’s relativity: –Special –General –Relativity and black holes Evidence of black holes Properties of black holes Long-time behavior of black holes

2. Special relativity Newton says space and time are perfectly uniform and unchanging. It is always possible to know exactly how fast you are moving through space and time. In 1905 Albert Einstein proposed his special theory of relativity describing how motion affects our measurements of distance and time. –Distances and time intervals measured depend on how the observer is moving. –Einstein’s theory is based on just two basic principles:

3. Principle 1 Your description of physical reality is the same regardless of the constant velocity at which you move. –The direction and actual speed don’t matter. You only need to have a constant velocity. –Called an inertial reference frame.

4. Principle 2 Regardless of your speed or direction of motion, you always measure the speed of light to be the same.

5. Consequences of special relativity Speed involves both distance and time. Since speed behaves differently in special relativity it shouldn’t be surprising that space and time behave differently as well. –In relativity space and time are intertwined in four-dimensional beast called spacetime. –Our perception of both length and time depend strongly on our motion.

6. Length contraction

7. Time dilation Moving clocks run slow.

8. Special relativity The astronaut with the flashlight will see the astronaut in the spaceship shortened in the direction of motion with a slowly ticking clock. These observations aren’t some sort of illusion. They are actual effects due to Einstein’s special relativity. Another important outcome of special relativity is E=mc 2.

9. General relativity Special relativity is a comprehensive description of light and, by extension, of electricity and magnetism. Einstein’s next goal was to develop a theory describing gravity. –His general theory of relativity did just this when published in 1915.

10. Equivalence principle In a small volume of space, the downward pull of gravity can be accurately and completely duplicated by an upward acceleration of the observer.

11. Equivalence principle This principle allowed Einstein to focus on motion rather than force. Einstein envisioned gravity as being caused by curvature of spacetime.

12. Testing general relativity

15. Relativity and black holes

16. Curved spacetime near a black hole

17. Detecting black holes X-ray source Cygnus X1 detected near B0 supergiant star. X-ray emissions are highly variable and flicker on 0.01 s timescale. –This means X-ray source is at most 3000 km in diameter. Cygnus X1 has estimated mass of 7 M . –Given its diameter it is likely a black hole.

18. X-rays from Cygnus X1

19. Vicinity of a rotating black hole

20. Supermassive black holes in galactic cores

21. Structure of a nonrotating black hole Event horizon: distance where escape speed just equals the speed of light Singularity: “region” where all of star’s mass has been crushed to zero volume (and infinite density) –Strength of gravity and curvature of spacetime are infinite at the singularity –Laws of physics don’t apply at the singularity. It’s a weird place.

22. Schwarzchild radius

23. Three properties of a black hole Once matter passes through the event horizon all information about it disappears except for three quantities: –Mass –Electric charge –Angular momentum

24. Structure of a rotating black hole

25. Evaporation of a black hole It is possible to get mass back out of a black hole through pair production. This happens faster with low mass black holes. –10 10 kg b.h. would need 15 billion years to evaporate while 5 M  b.h. would need 10 62 years.