Assignments. Read all (secs ) of DocOnotes-cosmology. HW7 due today; accepted till Thurs. w/ 5% penalty

Transcription

1 Assignments Read all (secs ) of DocOnotes-cosmology. HW7 due today; accepted till Thurs. w/ 5% penalty Term project due last day of class, Tues. May 17 Final Exam Thurs. May 19, 3:30 p.m. here

2 Olber s Paradox If Universe is infinite, then why is night sky black? in every direction, should eventually see a star sky should be ablaze with light Paradox solved by expanding Universe. Light gets redshifted to ever longer wavelengths Finite time => finite size => finite # stars Even such a simple observation -- the darkness of the night sky-- has profound implications!!

3 Olbers' Paradox If the universe were 1. infinite 2. unchanging 3. everywhere the same then stars would cover the night sky.

4 Olbers' Paradox If the universe were 1. infinite 2. unchanging 3. everywhere the same then stars would cover the night sky.

5 The night sky is dark because the universe changes with time. As we look out in space, we can look back to a time when there were no stars.

6 The night sky is dark because the universe changes with time. As we look out in space, we can look back to a time when there were no stars.

7 What have we learned? Why is the darkness of the night sky evidence for the Big Bang? If the universe were eternal, unchanging, and everywhere the same, the entire night sky would be covered with stars. The night sky is dark because we can see back to a time when there were no stars.

8 Running the Expansion Backward Early universe very crowded And very hot!

9 Recombination epoch Universe immersed in microwave radiation. Unleashed at the end of the Era of Nuclei. 380,000 years after Big Bang, Universe had cooled to 3000 K Free electrons became bound into atoms of H & He Recombination epoch without free electrons to scatter photons, Universe became transparent

10 The cosmic microwave background the radiation left over from the Big Bang was detected by Penzias and Wilson in 1965.

11 CMB Blackbody Spectrum

12 Background has perfect thermal radiation spectrum at temperature 2.73 K. Expansion of the universe has redshifted thermal radiation from that time to z~1100 times longer wavelength: microwaves.

13 Background radiation from the Big Bang has been freely streaming across the universe since atoms formed at temperature ~3000 K: visible/ir.

14 Planck CMB

15 CMB angular structure spectrum

16 How do observations of the cosmic microwave background support the big bang theory?

17 Scientific History of the Universe

18 The Planck satellite gives us detailed baby pictures of structure in the universe.

19 How do the abundances of elements support the Big Bang theory?

20 Protons and neutrons combined to make long-lasting helium 2015 Pearson nuclei when the universe was ~5 minutes Education, Inc. old.

21 Big Bang theory prediction: 75% H, 25% He (by mass) Matches observations of nearly primordial gases

22 Clicker Question Which of these abundance patterns is an unrealistic chemical composition for a star? A. 70% H, 28% He, 2% other B. 95% H, 5% He, less than 0.02% other C. 75% H, 25% He, less than 0.02% other D. 72% H, 27% He, 1% other

23 Clicker Question Which of these abundance patterns is an unrealistic chemical composition for a star? A. 70% H, 28% He, 2% other B. 95% H, 5% He, less than 0.02% other C. 75% H, 25% He, less than 0.02% other D. 72% H, 27% He, 1% other

24 Scientific History of the Universe

25 The Creation of Matter The early Universe was filled with radiation & subatomic particles. We ve seen matter converted to energy but Einstein s famous equation is a two-way street! E = m c 2 If T > K p + matter n e - p - n antimatter e +

26 Unification of Forces

27 Mysteries Needing Explanation 1. Where does structure come from? 2. Why is the overall distribution of matter so uniform? 3. Why is the density of the universe so close to the critical density? An early episode of rapid inflation can solve all three mysteries!

28 Inflation can make structure by stretching tiny quantum ripples to enormous sizes. These ripples in density then become the seeds for all structure in the universe.

29 How can microwave temperature be nearly identical on opposite sides of the sky?

30 Regions now on opposite sides of the sky were close together before inflation pushed them far apart.

31 Density = Critical Density > Critical The overall geometry of the universe is closely related to total density of matter and energy. Density < Critical

32 The inflation of the universe flattens the overall geometry like the inflation of a balloon, causing overall density of matter plus energy to be very close to critical density.

33 How can we test the idea of inflation?

34 Patterns of structure observed by WMAP show us the seeds of the universe.

35 Observed patterns of structure in the universe agree (so far) with the seeds that inflation would produce.

36 Seeds Inferred from CMB Overall geometry is flat Total mass + energy has critical density Ordinary matter ~5% of total Total matter is ~30% of total Dark matter is ~25% of total Dark energy is ~70% of total Age of 13.7 billion years In excellent agreement with observations of present-day universe and models involving inflation and WIMPs!

37 DocOnotes-cosmology.pdf

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40 Topology of Universe

41 Big Bang Nucleosynthesis

42 Big Bang Nucleosynthesis

43 Big Bang Nucleosynthesis