Chapter 17 Cosmology
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1 Chapter 17 Cosmology
2 Over one thousand galaxies visible
3 The Universe on the Largest Scales No evidence of structure on a scale larger than 200 Mpc On very large scales, the universe appears to be: Homogenous - the same everywhere Isotropic - the same in all directions
4 Figure 17.1 Galaxy Survey
5 Cosmology The study of the structure and evolution of the universe Cosmological principle - twin assumptions of homogeneity and isotropy Generally accepted by astronomers No edge (violates homogeneity) No center (violates isotropy)
6 Olbers s Paradox Assume that universe is infinite and unchanging in time When you look at sky at night, your line of sight will eventually encounter the bright surface of a star Entire sky should be as bright as the sun But sky is dark at night - Olbers s Paradox From nineteenth century Heinrich Olbers
7 Figure 17.2 Olbers s Paradox
8 Analogy 17-1 Every sight line intersects a tree
9 Olbers s Paradox Since sky is dark at night, either universe is not infinite and/or universe evolves in time
10 Hubble s Law Recession velocity = H 0 X distance How long did it take a galaxy to reach its current distance from us? Distance = velocity X time time = Distance/velocity = Distance/(H 0 X distance) = 1/H 0 = 14 billion years (for H 0 = 70 km/s/mpc)
11 Birth of the Universe Hubble s law implies that 14 billion years ago, all galaxies were at the same location Everything in the universe was confined to a single point then The point exploded - this is the Big Bang This was the beginning of the universe and the beginning of time
12 Big Bang Big Bang explains Olbers s paradox - even if universe is infinite, we only see a finite part within 14 billion light-years Light from beyond has not yet reached us
13 Where was Big Bang? Big Bang was not an explosion of matter into space Big Bang was an explosion of the universe itself, or of space itself Galaxies don t rush into empty space - instead space itself expands Entire universe was a point - the Big Bang happened everywhere at once
14 Receding galaxies Think of galaxies as coins taped to an expanding balloon Surface of balloon represents universe Every coin sees every other coin recede No coin is at center
15 Figure 17.3 Receding Galaxies
16 Cosmological Redshift For expanding universe, Doppler interpretation not technically correct Galaxies are not moving apart through space Instead, space itself is expanding Redshift represents expansion of wavelength as universe expands
17 Figure 17.4 Cosmological Redshift
18 Fate of the Universe Will universe expand forever? Similar to escape velocity from a planet Will object tossed upward rise forever or fall back? Depends on launch speed and mass of planet
19 Figure 17.5 Escape Speed
20 Critical Density Low density universe expands forever High density universe collapses in a Big Crunch Critical Density is the dividing line For H 0 = 70 km/s/mpc, critical density is 9 X kg/m Milky Way galaxies per cubic Mpc
21 Figure 17.6 Model Universes
22 Geometry of space Mass/energy warps space The greater the total density, the greater the curvature Density includes mass (visible and dark matter) Also includes all energy
23 Cosmic density parameter 0 is ratio of actual to critical density 0 > 1.0 is a closed universe 0 < 1.0 is an open universe 0 = 1.0 is a critical universe
24 Flat space Euclidean geometry Parallel lines never meet Angles in triangle add to 180 Circumference of circle is 0 = 1, critical universe Infinite in extent X diameter
25 Positively curved space Studied by Georg Riemann Like surface of sphere Parallel lines intersect twice Angles in triangle add to more than 180 Circumference of circle is < 0 > 1, closed universe Finite in extent X diameter
26 Figure 17.7 Einstein s Curve Ball - Closed Universe
27 Negatively curved space Studied by Nikolai Lobachevsky Imagine a saddle shape Infinite number of lines through a point parallel to another line Angles in triangle add to less than 180 Circumference of circle is > 0 < 1, open universe Infinite in extent X diameter
28 More Precisely 17.1 Curved Space
29 Cosmic density parameter Counting all luminous matter gives several percent Adding in estimated dark matter in galaxies and clusters gives On a larger scale distribution of dark matter not well known 0 of Overall cosmic density less than critical
30 Cosmic acceleration Use Type I supernovae to measure distances (independent of Hubble s law) If gravity slowing expansion - universe is decelerating - objects at great distances - (long ago) - should be receding faster than Hubble s law predicts Data seems to show expansion is accelerating
31 Figure 17.8 Accelerating Universe
32 Cosmic acceleration What causes this acceleration? Dark energy - exerts repulsive force Dark energy may greatly exceed total mass (luminous and dark) of universe
33 Cosmological Constant Vacuum pressure force associated with empty space First suggested by Einstein in his equations showed universe evolved in time Expansion of universe not known then When discovered, he discarded Cosmologial Constant as the biggest mistake of his scientific career May be making a comeback as a dark energy explanation
34 Discovery 17-1 Einstein and the Cosmological Constant
35 Cosmic Composition Theoretical studies suggest universe is flat A variety of measurements lead to 0 = 1.0 Density is made of both matter (27%) and dark energy (73%) Gravity tends to slow expansion Dark energy tends to increase expansion Universe will expand forever
36 Figure 17.9 Geometry of the Universe
37 Age of universe For H 0 = 70 km/s/mpc, Age of critical density universe with no cosmological constant is 9 billion years Age of low density universe > 9 billion y Age of high density universe < 9 billion y Age of accelerating universe is about 14 billion y
38 Figure Cosmic Age
39 Age of universe Globular clusters formed billion years ago Consistent with 14 billion years age for universe with 2 billion years for galaxies to evolve Inconsistent with critical density with no dark energy
40 Cosmic Microwave Background Penzias and Wilson in 1964 discovered a hiss in all directions of space Microwave wavelengths - blackbody curve at 2.7 K Gamma ray wavelengths in early universe cosmologically redshifted to microwave wavelengths Radiation is isotropic (same in all directions) Contains far more energy than all of energy emitted by all stars and galaxies
41 Figure Microwave Background Discoverers
42 Figure Cosmic Blackbody Curves
43 Figure Microwave Background Spectrum
44 Matter and Radiation Currently density of matter much greater than density of radiation Matter-dominated universe In past, both radiation and matter more dense But radiation cosmologically redshifted Early universe radiation-dominated
45 Figure Radiation-Matter Dominance
46 Formation of nuclei and atoms Early universe almost entirely radiation In first minute photons had sufficient energy to transform into electrons, protons, neutrons and exotic particles Primordial nucleosynthesis - formation of elements heavier than hydrogen shortly after Big Bang
47 Deuterium and helium Below 900 million K, about two minutes after Big Bang, protons and neutrons fused into deuterium After short while, deuterium fused into heavier elements, mostly He-4 Almost all neutrons consumed By 15 minutes, elemental abundance set
48 Figure Helium Formation
49 Deuterium abundance Not all primordial deuterium converted to He Present day density of universe indicated by deuterium remaining Gives density of normal matter of 3 to 4 percent of critical Total matter density is about 1/3 of critical Most of matter is dark and not composed of protons and neutrons
50 Formation of Atoms At age of tens of thousands of years, matter began to dominate over radiation Cooled enough for nuclei and electrons to form atoms - known as de-coupling Before then, free electrons scattered radiation Universe went from opaque to transparent After about 400,000 years, temperature fell to 3000 K, and microwave background we see now released when universe was 1100X smaller than today
51 Figure Radiation-Matter Decoupling
52 Horizon Problem Observe two regions at opposite directions in sky Microwave background same at both Density and temperature same at both But not enough time, even at speed of light, to connect them
53 Figure Horizon Problem
54 Flatness Problem Universe is very close to being flat today Universe must have been extremely close to critical in the past Why is universe s density nearly critical, out of all possibilities?
55 Figure Flatness Problem
56 Horizon and Flatness problems explained Grand Unified Theory (GUT) describes superforce made up of electromagnetism and strong and weak nuclear forces 3 forces unified at very high temperatures Predicts that at s after Big Bang, at K, universe greatly expanded by factor of until s Epoch of inflation
57 Figure Cosmic Inflation
58 Cosmic inflation Explains horizon problem Inflation took parts of universe that had communicated, then dragged them far apart Explains flatness problem Curved space, greatly expanded, appears flat
59 Figure Inflation and the Flatness Problem
60 Formation of large-scale structure Small inhomogeneities in early universe grew into large scale structures Dark matter, unaffected by radiation, clumped and gravitationally affected normal matter
61 Figure Structure Formation
62 Figure Structure Simulated
63 COBE map Dark matter doesn t emit or absorb radiation Its gravity affects redshift of cosmic microwave background radiation Measured by COBE satellite Map shows universe is of critical density
64 Figure Cosmic Microwave Background Map
65 Figure Early Structure - WMAP spacecraft
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