a brief tour of the universe don’t panic the sun in uv

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  • Slide 1
  • Slide 2
  • A Brief Tour of the Universe Dont Panic
  • Slide 3
  • The Sun in UV
  • Slide 4
  • Some Distances Distance to moon 10 times around the earth 1.3 light seconds Sun 400 times the distance to the moon 8.3 light minutes Nearest star 4.2 light years Andromeda galaxy 2.5 million light years
  • Slide 5
  • A Fruity Comparison If the sun were a grapefruit and all other distances were scaled accordingly The earth would be a pinhead 10 meters away. The nearest star would be 2000 miles away.
  • Slide 6
  • Slide 7
  • The Milky Way Galaxy 100,000 light years in diameter 225 million years rotation period 100 billion stars as many sand grains as there are in one meter cube. It would take you 3000 years to count them.
  • Slide 8
  • A More Comparisons If the earths orbit were the size of a pinhead and all other distances were scaled accordingly The nearest star would be 300 yards away. Our galaxy would span the entire United States.
  • Slide 9
  • Galaxy Cluster
  • Slide 10
  • Slide 11
  • Final Comparisons If the milky way were 20 yards across -- Andromeda would be 600 yards away. The farthest distance we could see would be the size of the United States and contain 100 billion galaxies.
  • Slide 12
  • Slide 13
  • Hubble Plot Recession Speed vs. Distance
  • Slide 14
  • The Hubble Constant The Hubble Time ~ the age of the universe
  • Slide 15
  • Slide 16
  • Slide 17
  • The Cosmological Principle Everything is at the center!
  • Slide 18
  • 18 Geometry on a sphere
  • Slide 19
  • 19 R(t 2 ) * * * * time = t 1 time = t 2 Space is expanding: The distance from here to there keeps getting farther. Space is expanding: The distance from here to there keeps getting farther. R(t 1 )
  • Slide 20
  • 20 Simple solutions to Friedmans equations R(t) t scale factor time k= +1 k=0 k= -1 Big BangBig Crunch now
  • Slide 21
  • Critical density The critical density is equivalent to six hydrogen atoms per cubic meter. If the density of the universe is less than this it will expand forever. If the density is greater, it will re-collapse.
  • Slide 22
  • 22 Shape #1: spherical, closed geometry finite, unbound k = +1 l General Relativity: the Universe can have only one of three possible shapes
  • Slide 23
  • 23 Shape #2: saddle-shaped, open geometry infinite, unbound k = -1 l
  • Slide 24
  • 24 Shape #3: flat or Euclidean geometry infinite, unbound (unbound = no edge) k = 0 l But the Universe has shape #3
  • Slide 25
  • The three Scenarios: k=+1 The density of the universe is greater than the critical density. The universe will expand for a while and then re-collapse in the big crunch. The curvature is positive like the surface of a sphere. All straight lines eventually come back to where they started.
  • Slide 26
  • The three scenarios: k=-1 The density of the universe is less than the critical density. The universe will go on expanding forever. Space has negative curvature, e.g.
  • Slide 27
  • The three scenarios: k=0 The universe has exactly the critical density. The universe will go on expanding, but the expansion will eventually coast to a stop. Euclid was right. As a matter of fact, space is flat. And yet the density of matter that we can see is much less than the critical density.
  • Slide 28
  • Slide 29
  • 29 Energy Content of the Universe + baryons + dark matter + dark energy = crit = 1 k = 0
  • Slide 30
  • Summary So Far The universe is infinite (so far as we know). It has flat, Euclidean geometry. Its expanding. If it has always expanded at the same rate, there would have been a time 13.5 billion years ago when everything we can now see was compressed to a point.
  • Slide 31
  • When matter (or radiation) is compressed, it heats up. When it expands it cools down. So what is the temperature of the universe now?
  • Slide 32
  • 2.73 degrees K Now run the clock backwards, starting now.
  • Slide 33
  • t=350,000 years a.b.b. T=3000 degrees Neutral hydrogen breaks up to form electrons and protons. So the universe is no longer transparent.
  • Slide 34
  • The Universe As Seen from the Outside But heres what we see the cosmic microwave background
  • Slide 35
  • t=3 minutes a.b.b. T= one billion degrees The only nuclei around are isotopes of hydrogen, helium, and a smidgeon of lithium. These now break up to make protons and neutrons.
  • Slide 36
  • t=one second a.b.b. Protons and neutrons break up to make quarks.
  • Slide 37
  • This is the realm of quantum gravity. We have no idea what happened before this time.
  • Slide 38
  • Five Things That Had To Be Exactly Right Critical Density
  • Slide 39
  • Slide 40
  • How Light Nuclei Are Formed
  • Slide 41
  • How Stars Make Energy
  • Slide 42
  • What Could Go Wrong If the strong force were slightly stronger the universe would only consist of protons and di- protons. If it were slightly weaker there would be no deuterons and stars couldnt shine.
  • Slide 43
  • Five Things That Had To Be Exactly Right Critical Density The strong force
  • Slide 44
  • How Stars Make Heavy Elements etc.
  • Slide 45
  • Until It Makes Iron
  • Slide 46
  • And Then
  • Slide 47
  • Slide 48
  • Ashes to ashes, dust to dust
  • Slide 49
  • And Then New Stars
  • Slide 50
  • Slide 51
  • Five Things That Had To Be Exactly Right Critical Density The strong force The structure of
  • Slide 52
  • The cosmic microwave background Galaxy clusters are seeded by small variations in density.
  • Slide 53
  • Five Things That Had To Be Exactly Right Critical Density The strong force The structure of The strength and scale of the fluctuations
  • Slide 54
  • Antimatter??? Presumably the universe started out with an equal number of particles and antiparticles. All the particles and antiparticles should then annihilate leaving nothing but photons. This almost happened. There are a billion photons for every proton. This doesnt make sense!
  • Slide 55
  • Life only works in three dimensions. There can be no networks in two dimensions. There can be no stable planetary orbits in higher dimensions.
  • Slide 56
  • Five Things That Had To Be Exactly Right Critical Density The strong force The structure of The strength and scale of the fluctuations Space has three dimensions.
  • Slide 57
  • Anthropic principles The weak anthropic principle: since we exist the universe must have the properties necessary for our existence. The strong anthropic principle: the universe must have the properties necessary for our existence.
  • Slide 58
  • The final word Whereof one cannot speak, one must be silent. Ludwig Wittgenstein