10B The Big Bang Where do we come from, where are we going?
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Transcript of 10B The Big Bang Where do we come from, where are we going?
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The Big BangThe Big Bang
Where do we come from, where are we going?
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GoalsGoals
• What’s the cosmological principle?• Where did things begin?• Where will things end?• What’s the temperature of space?
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Hubble’s Law
• Recall: All galaxies are moving away from us.
• The farther away the faster they go.
• V = Ho x D
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You Are Here
Large Scale StructureFarther away we look, further back in time we see!
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Cosmological Principle
• Isotropy – The view from here is the same in all directions.
• Homogeneity – We live in an average place the same as any other.
• This is the cosmological principle.
• Implies: – Universe has no edge!– Universe has no center!
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Olber’s Paradox
• Why is it dark at night?
• In an infinite and unchanging universe:Every line of sight should end at the surface of a star.
• Universe is neither.
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Expanding Universe• If galaxies are all moving away, then at
some point they were all much closer.• Hubble’s Law implies the Universe is
expanding.
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Age of the Universe• Since all galaxies are moving away
from us, how long has it been since all galaxies were together?time = distance / velocityvelocity = Ho x distance
time = distance / (Ho x distance)
time = 1/Ho
• Measured Ho ~ 65 km/s/MpcT ~ 15 billion years
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Age Disagreements
• Until recently, much disagreement on the value of Ho and therefore, the age of the Universe.
• Need to know the distance to some galaxies in order to know the slope of velocity versus distance.
• Different methods yielded different distances.
• Some values of Ho yielded an Universe younger than some of its stars.
• HST has helped solve the problem: Cepheids.
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The Big Bang• Big Bang: the explosion out of which
the Universe began expanding.• Into what did the Universe expand?
Nothing.• Where was the Big Bang? Everywhere.• Where is the center of the Universe?
Nowhere.
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The End of the Universe
• Will the universe expand forever?
• Depends on the density of the Universe.
• Too big: Big Crunch– Closed Universe– Bound Universe
• Too small: Big Freeze– Open Universe– Unbound Universe
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Critical Density
• Dividing line is the critical density.
o is the ratio of measured density to the critical density.
• If o > 1 then closed, o < 1 then open.
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Density of the Universe
• Add up all the mass we see and o = 0.01
• But we know there is some dark matter in galaxies and clusters.
• How much?• Think ~10 x more dark matter than
“light” matter.
• Cosmologists think o < 0.3
• Result: Open Universe Big Freeze!
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Are we Slowing down?• In our experience,
things slow down over time.
• Is the Universe slowing down at all?
• Use supernovae as “standard candles.”– Get distance to
distant supernovae.
• Plot distance versus velocity.
Slowing
Accelerating
Dark Energy
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Observational Clues• Instant of the Big Bang:
– Very Dense– Very hot
• Universe one giant blackbody.– Temperatures gamma rays
• As space expands, wavelengths of light expand with it Cosmological Redshift
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3 Kelvin
• Recall: p 1/T
• Since longer wavelengths mean cooler blackbodies then space should be cooling.
• Today, it should be ~3 K
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COBE
• Satellite measured the intensity of energy from space at a range of frequencies.
2.7 K
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Isotropy
• Amazingly uniform temperature in all directions.
• Deviations < 0.0002 Kelvin
10 x more energy in background than everywhere else.