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ASTR100 (Spring 2008) Introduction to AstronomyCosmological Inflation
Prof. D.C. Richardson
Sections 0101-106
An early episode of rapid inflation can solve all three mysteries!
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? That is, why does the universe have
such a flat geometry?
Inflation can make structure by stretching tiny quantum ripples to enormous size.
These ripples in density then become the seeds for all structure in the universe.
Regions now on opposite sides of the sky were close together before inflation pushed them far apart.
The overall geometry of the universe is closely related to total density of matter and energy.
Density = Critical
Density > Critical
Density < Critical
Inflation of universe flattens overall geometry, causing total density of matter plus energy to be very close to critical density.
In excellent agreement with observations of present-day universe and models involving inflation and WIMPs!
“Seeds” Inferred from CMB
Overall geometry is flat. Total mass + energy has critical density.
Total matter is ~ 26% of total. Ordinary matter ~ 4.4% of total. Dark matter is ~ 22% of total.
Dark energy is ~ 74% of total. Universe is 13.7 billion years old.
Olbers’ Paradox
If universe were
1) infinite;
2) unchanging;
3) everywhere the same;
then, stars would cover the night sky.
Olbers’ Paradox
If universe were
1) infinite;
2) unchanging;
3) everywhere the same;
then, stars would cover the night sky.
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.
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.
Cool fact: if you tune your TV set between channels, a few percent of the "snow" that you see on your screen is noise caused by the background of microwaves…
The Drake Equation
Number of civilizations with whom we could potentially communicate
= NHP flife fciv fnow
NHP = total number of habitable planets in galaxy;
flife = fraction of habitable planets with life;
fciv = fraction of life-bearing planets with civilization at some time;
fnow = fraction of civilizations around now.
We do not know the following values for the Drake equation:
NHP : probably billions.
flife : ??? hard to say (near 0 or near 1).
fciv : ??? it took 4 billion years on Earth.
fnow : ??? can civilizations survive long-term?
We’ve even sent a few signals
ourselves…
Earth to globular cluster M13: Hoping we’ll hear back in about 42,000 years!
Pioneer plaque Voyager record
Current Spacecraft
Current spacecraft travel at <1/10,000 c; 100,000 years to the nearest stars.
ASTR100 (Spring 2008) Introduction to AstronomyCourse Review
Prof. D.C. Richardson
Sections 0101-0106
Chapter Summaries
1. Our Place in the Universe2. Discovering the Universe for
Yourself3. The Science of Astronomy4. Making Sense of the Universe5. Light: The Cosmic Messenger6. Formation of Planetary Systems7. Earth and the Terrestrial Worlds8. Jovian Planet Systems9. Asteroids, Comets, and Dwarf
Planets
Chapter Summaries
10. Our Star11. Surveying the Stars12. Star Stuff13. The Bizarre Stellar Graveyard14. Our Galaxy15. Galaxies and Cosmology16. Dark Matter, Dark Energy, and
the Fate of the Universe17. The Beginning of Time18. Life in the Universe
Latest Material (Ch. 12–14)
Star Stuff Star birth. Stellar evolution (low-mass vs. high-mass). Planetary nebulae, massive star supernovae.
The Bizarre Stellar Graveyard White dwarfs, neutron stars, black holes. Novae, white dwarf supernovae, pulsars. Gamma ray bursts (skipped).
Our Galaxy Structure, star-gas-star cycle, formation. Galactic center.
Latest Material (Ch. 15–17)
Galaxies and Cosmology Galaxy types, distances, evolution. Hubble’s Law. Quasars and other Active Galactic Nuclei.
Dark Matter, Dark Energy, and the Fate of the Universe Dark matter: nature, evidence. Structure formation. Fate of the universe, dark energy.
The Beginning of Time The Big Bang, evidence, inflation.
Final Exam
Fri May 16, 8 am – 10 am, this room. Don’t be late! And DON’T miss the exam!! Special needs: go to Shoemaker, same time.
Chapters 1 through 17 inclusive. Most weight on chapters 12–15. No notes, calculators, cell phones, etc.
Worth 120 points (~22%)… 48 × 1-2/3 for multiple choice. 4 × 10 for short answer (night sky, planets, stars, galaxies).
5-pt bonus!