BIG BANG

1. BIG BANG

2. EVIDENCE FOR BIG BANG

3. Hot Big Bang Model: The universe began expanding a finite time ago from a very dense, very hotinitial state. Dense = particles packed close together. Hot= particles moving rapidly. As space expanded, the universe became lower in densityandcolder. Expansion of space has been continuous since the big bang (start of expansion).

4. “BigBang”is a rather misleading name. Galaxies are not flying throughspace like shrapnel after an explosion. They move apartcarried alongwithexpanding space.

5. Top pieces of evidence for the Hot Big Bang. 1)Darknight sky → Finite age for the universe. 2)Redshiftproportional to distance → Homogeneous and isotropic expansion. 3)Cosmic Microwave Background → Universe was hot & dense enough to be opaque.

6. Other evidence for the Hot Big Bang. 4)¼ helium + ¾ hydrogen→ Universe was hot and dense enough for early nucleosynthesis. 5) Age measurementsof stars and planets are less than the Hubble time 1/H0 . 6)Large scale structure looks like that seen in simulations of an expanding universe.

7. COSMIC MICROWAVES CMB= light left over from early, hot, dense, opaque universe. The universe became transparentwhen scale factor wasa ≈ 1/1000, and the time was t ≈ 400,000 years. From then until now (t ≈ 14 billion years), CMB photons have been freely moving..

8. Observing the CMB: COBE WMAP COBE (1989) WMAP (2003) Water vapor in Earth’s atmosphere absorbs microwaves: go abovethe atmosphere!

10. 1% of the specks on any TV tuned between stations are interactions with the big bang.

11. STRUCTURE FORMATION

12. Observation: After subtracting the effect of our motion through space, the CMB still shows hot and cold spots, about 1 degree across. Temperature fluctuation = 1 part per 100,000

13. Interpretation: observed temperature fluctuations result from the densityfluctuations in the early universe. Regions that were compressed had higher density, but also higher temperature (gases heat up as they are compressed). Hot spots in the CMB are higher in temperature than cold spots by only 1 part per 100,000. So the densityfluctuationsin the early universe were also small (about 1 part per 100,000).

14. Galaxies form from a hot, dense, smooth state.

15. 2 1 3 4 Matter distribution goes from smooth to lumpy.

16. Great Oaks from Tiny Acorns Grow. A dense region will become denser&more massivewith time; its gravity attracts surrounding matter. The Rich Get Richer, the Poor Get Poorer. A region that was slightly denser than average will eventually become much denser than average; it’s compressed by its own gravity.

17. It’s possible (with a very big computer) to simulate the steady growth of density fluctuations due to gravity. M1 M2 R2 F = • Make a large (imaginary) box. • Fill it with (simulated) massive particles. • Start with a nearly smooth distribution. • Let gravity act for billions of years.

18. then now The size of the box grows from 1.5 Mpc to 43 Mpc. redshift 0 13 billion years ago now It’s a few 100 million years before galaxies form.

19. Geshe Activity For the most ambitious activity, Geshes will be responsible for simulating structure formation. We will start with a nearly smooth distribution of “particles,” allow gravity to act, and watch the changing pattern over intervals of time.

20. MONK GRAVITY MODEL

21. RULES OF THE GAME • The black plastic disks are particles in the universe. Think of them as the galaxies. • We will evolve the distribution in steps of time, moving each disk once each step • The direction of motion of each move is given by the sum of the neighbor’s gravity. • Each move is a disk width, directed to the arrow oriented according to the gravity. • The starting situation is close to smooth, but random and not exactly uniform.

22. Inverse Square Law Force = X Force = 4X Force = 2X Force = 6X

23. UNIFORM

24. RANDOM

25. EASY  ?

26. HARDER  ?

27. REALLY HARD  ?

28. Move it a disk width in arrow direction Turn it over to show it’s been moved  