1 / 22

Atmospheric CO 2 reaches 400 PPM

Atmospheric CO 2 reaches 400 PPM. AST101 Lecture 28 The End of the Universe. Most Recent Numbers. H 0 = 67.8 ± 0.8 km/s/Mpc Ω = 0.9995 ± 0.0034 (universe is flat) Age of the universe: 13.798 ± 0.037 Gyr Ω Λ = 0.692 ± 0.010 Ω B = 0.048 ± 0.001 Ω DM =0.260 ± 0.004

aurora-mcdowell
Download Presentation

Atmospheric CO 2 reaches 400 PPM

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Atmospheric CO2 reaches 400 PPM

  2. AST101Lecture 28The End of the Universe

  3. Most Recent Numbers • H0 = 67.8 ± 0.8 km/s/Mpc • Ω = 0.9995 ± 0.0034 (universe is flat) • Age of the universe: 13.798 ± 0.037 Gyr • ΩΛ = 0.692 ± 0.010 • ΩB = 0.048 ± 0.001 • ΩDM =0.260 ± 0.004 Data from Planck release 1

  4. General Relativity Gμν = 8πTμν • Gμν: gravitational field • Tμν: stress-energy tensor

  5. The Vacuum Energy • If the vacuum exerts a pressure, it must have mass, and an energy density ρv • ab-initio calculations  ρv>1091 erg/cm3 • Inflation  ρv>1071 erg/cm3 • Today: ρv~ 0 • ρv<ρcrit • SNe  ρv~ 0.7 ρcrit, or ~ 6 x 10-30 erg/cm3 Note the discrepancy of ~10120

  6. How the Universe Expands

  7. The Equation of State of Dark Energy • Equation of state: pressure = wx density. • Ordinary matter: w = 0 (ρ ~ 1/V ~ a-3) • Relativistic matter: w = 1/3 (ρ ~ a-4) • Possibilities for Dark Energy: • Cosmological constant: constant pressure (w =-1) • Quintessence: a relaxing quantum field (-1/3 > w > -1) • Exotic solid matter: strings and walls (w = -1/3, -2/3) • Phantom energy: repulsive gravity (w < -1)

  8. The Equation of State of Dark Energy Constraints on w from the CMB and SNe observations

  9. Is this a privileged time? • 10 Gya: ΩΛ = 0.09 • Today: ΩΛ = 0.73 • In 10 Gyr: ΩΛ = 0.96

  10. The Multiverse • The universe is very improbable • Why did the universe turn out the way it did? • Perhaps there are other universes, each with their own set of physical constants • String theory suggests there may be ~10500 distinct universes

  11. Standard Model Free Parameters • 12 fermion masses (including 3 neutrinos) • 7 CKM mixing angles + 1 phase • electromagnetic coupling constant α • strong coupling constant αs • weak coupling constant GF = 1.16637×10-5 GeV-2 • Z0 mass mZ= 91.1876 GeV/c2 • Higgs mass • ➜25 free parameters (61 particles; 4 forces)

  12. Th. Wright, 1751

  13. The Anthropic Principle The universe is the way it is because, if it wasn’t, we would not be here to consider the question.

  14. Fire and Ice Some say the world will end in fire,Some say in ice.From what I've tasted of desireI hold with those who favor fire.But if it had to perish twice,I think I know enough of hateTo say that for destruction iceIs also greatAnd would suffice. Robert Frost 1920

  15. The End of the Universe Today, the universe is 13.7 billion years old. • 15 Gyr. (1 billion years from now). The increasing solar luminosity makes the Earthuninhabitable. • 19 Gyr. (5 billion years from now). The Sun leaves the main sequence. Mercury is vaporized. The planets spiral outwards as the red giant Sun loses mass in a solar wind. Venus may survive; the Earth ends up near where Mars is now. • 21 Gyr. (7 billion years from now). The Sun becomes a white dwarf. • 1012-13 yrs. The lowest mass stars burn out and become white dwarfs. Galaxies in clusters merge. • 1013-14 years. There are no luminous stars. The stelliferous ends; we enter the degenerate era.

  16. The End of the Universe The Degenerate Era • 1014 yrs. Universal expansion has carried all galaxies out of sight. It is a lonely universe. • 1014-33 yrs. All matter is in black holes, neutron stars, white dwarfs, brown dwarfs, and planets. • 1016-20 yrs. Collisions strip planets from stars, and eject stars from galaxies. Central black holes grow. • 1014-20 yrs. • Binary stars spiral together and merge. • Collisions between white dwarfs produce supernovae. • Collisions between brown dwarfs produce low mass stars. • Typical galaxies shine with one solar luminosity.

  17. The End of the Universe The Degenerate Era • 1020 yrs. The only luminosity in the universe comes from white dwarfs absorbing dark matter. White dwarfs glow at a temperature of 64K. • 1033-37 yrs. The end of matter. Protons decay. White dwarfs glow with an luminosity of 400 Watts. • >1060 yrs. The Black Hole era begins. • 1065 yrs. Stellar mass black holes evaporate. • 10100 yrs. Galactic mass black holes evaporate.

  18. The End of the Universe • >10100 yrs: the universe is a dilute and ever-expanding gas of photons, neutrinos, electrons, and their antiparticles. • Eventually all particles annihilate with their antiparticles. This is how the world will end. Not with a bang, but a whimper.

  19. The End of the Universe What if w < -1? (phantom energy) • 35 Gyr: the Big Rip tears the universe apart • Big Rip timeline : • T0 - 60 million years: the Milky Way is torn apart. • T0 - 3 months: the solar system is unbound. • T0 - 30 minutes: the Earth explodes. • T0 - 15 seconds: atoms are pulled apart. Caldwell et al., Phys Rev Letters, August 15 2003

  20. Reference This timeline has been adapted, in part, from The Future of the Universe, by F.C. Adams and G. Laughlin, Sky and Telescope, August 1996, pg. 32, and from The Anthropic Cosmological Principle, by J.D. Barrow and F.J. Tipler, 1986 (Oxford University press).

More Related