Exploring the Early Universe

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Exploring the Early Universe

• Chapter Twenty-Seven

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Guiding Questions

1. Has the universe always expanded as it does
   today, or might it have suddenly inflated?
2. How did the fundamental forces of nature and the
   properties of empty space change during the first
   second after the Big Bang?
3. What is antimatter? How can it be created, and
   how is it destroyed?
4. Why is antimatter so rare today?
5. What materials in todays universe are remnants
   of nuclear reactions in the hot early universe?
6. How did the first galaxies form?
7. Are scientists close to developing an
   all-encompassing theory of everything?

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Standard Big Bang Has Problems

• Flatness problem
• Observational tests suggest that universe is
  astonishingly close to the flat Friedmann
  universe, which is the least probable one.
• Homogeneity problem
• CMBR coming from 13.7 x 109 light years in one
  direction is incredibly like that coming from
  13.7 billion light years in any other direction.

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17.3 The Big Bang and Inflation

1. What aspects of the universe were originally
   unexplained by the Big Bang model?
2. Who does inflation explain these features of the
   universe?
3. How can we test the idea of inflation?

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How can CMBR temperature be nearly identical on
opposite sides of the sky?
time
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The Isotropy Problem
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The newborn universe may have undergone a brief
period of vigorous expansion

• A brief period of rapid expansion, called
  inflation, is thought to have occurred
  immediately after the Big Bang
• During a tiny fraction of a second, the universe
  expanded to a size many times larger than it
  would have reached through its normal expansion
  rate

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Inflationary Epoch

• 1980s, Alan Guth proposed inflationary epoch
  could account for flatness and homogeneity
  problems.
• Epoch began at 10-35 s and lasted 10-24-36 s
• Extremely small portion of universe ballooned
  outward in all directions at speeds greater than
  the speed of light
• Expanded by 1030-50 times to become visible
  universe of today
• Inflated portion pushed other material far beyond
  its boundaries

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Inflation Stretching of Spacetime Ripples

• Grand unified theories predict that the
  separation of the strong force from the GUT force
  should have released enormous amounts of energy.
• During inflation, ripples in spacetime would have
  stretched by a factor of perhaps 1030. Peaks of
  these ripples would have become the density
  enhancements that produced all structure we see
  in the universe today.

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How Inflation Solves Homogeneity Problem
Inflation explains large-scale uniformity by
saying that distant regions of our observable
universe today were once close enough to exchange
radiation (information about their physical
state).
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Inflation explains why the universe is nearly
flat and the 2.725-K microwave background is
almost perfectly isotropic
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Inflation was one of several profound changes
thatoccurred in the very early universe

• Four basic forcesgravity, electromagnetism, the
  strong force, and the weak forceexplain all the
  interactions observed in the universe

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• Grand unified theories (GUTs) are attempts to
  explain three of the forces in terms of a single
  consistent set of physical laws
• A supergrand unified theory would explain all
  four forces
• GUTs suggest that all four physical forces were
  equivalent just after the Big Bang

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• However, because we have no satisfactory
  supergrand unified theory, we can as yet say
  nothing about the nature of the universe during
  this period before the Planck time (t 1043 s
  after the Big Bang)
• At the Planck time, gravity froze out to become a
  distinctive force in a spontaneous symmetry
  breaking
• During a second spontaneous symmetry breaking,
  the strong nuclear force became a distinct force
• This transition triggered the rapid inflation of
  the universe
• A final spontaneous symmetry breaking separated
  the electromagnetic force from the weak nuclear
  force from that moment on, the universe behaved
  as it does today

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During inflation, all the mass and energy inthe
universe burst forth from the vacuum of space

• Heisenbergs uncertainty principle states that
  the amount of uncertainty in the mass of a
  subatomic particle increases as it is observed
  for shorter and shorter time periods
• Because of the uncertainty principle,
  particle-antiparticle pairs can spontaneously
  form and disappear within a fraction of a second
• These pairs, whose presence can be detected only
  indirectly, are called virtual pairs

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As the early universe expanded and cooled, most
of the matter and antimatter annihilated each
other

• A virtual pair can become a real
  particle-antiparticle pair when high-energy
  photons collide
• In this process, called pair production, the
  photons disappear, and their energy is replaced
  by the mass of the particle-antiparticle pair
• In the process of annihilation, a colliding
  particle-antiparticle pair disappears and high
  energy photons appear
• Need to show figure 2710 on p 730.

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The Origin of Matter - Nucleosynthesis

• Just after the inflationary epoch, the universe
  was filled with particles and antiparticles
  formed by pair production and with numerous
  high-energy photons formed by annihilation
• A state of thermal equilibrium existed in this
  hot plasma
• As the universe expanded, its temperature
  decreased
• When the temperature fell below the threshold
  temperature required to produce each kind of
  particle, annihilation of that kind of particle
  began to dominate over production
• Matter is much more prevalent than antimatter in
  the present day universe
• This is because particles and antiparticles were
  not created in exactly equal numbers just after
  the Planck time

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A background of neutrinos and most of the
heliumin the universe are relics of the
primordial fireball

• Helium could not have been produced until the
  cosmological redshift eliminated most of the
  high-energy photons
• These photons created a deuterium bottleneck by
  breaking down deuterons before they could combine
  to form helium

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The abundance of helium in the universe is
explained by the high temperatures in its early
history
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Helium Synthesis
Calculations show that protons outnumbered
neutrons 7 to 1 during nucleosynthesis era or 12
hydrogen nuclei for each helium nucleus. Thus,
the H/He mass ratio is 12 to 4 or 75 to 25.
Agreement between this prediction and the
observed abundance of helium is important
evidence in favor or Big Bang evolution.
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Measured Abundances of H2, He3, and Li7
Abundances of other light elements agree with Big
Bang model having 4 normal baryonic matter
rest of 27 matter is dark matter!
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Nuclei produced between 10 seconds and 10 hrs
after Big Bang
Nucleosynthesis is stabilized at about 1000
seconds or 15 minutes after BB
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Globular clusters are believed to be among the
first objects to form in the universe.
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Galaxies formed from density fluctuations in the
early universe (simulation)
Z 3.04 corresponding to 2.2 billion years after
big bang
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Astronomers use supercomputers to simulate how
the large-scale structure of the universe arose
from primordial density fluctuations
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Building blocks of galaxies form from the
bottoms up agreeing with dark Matter basis of
coalescing of large scale structures. Green color
are redshifted From ultraviolet photons.
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IR 1916 has a z 10! It is only about 3000 light
years across, about 1/10 the Size of the Milky
Way. It is a possible galaxy building block.
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Models based on dark energy and cold dark matter
give good agreement with details of the
large-scale structure
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Summary of evolution of Universe
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Theories that attempt to unify the physical
forcespredict that the universe may have 11
dimensions

• The search for a theory that unifies gravity with
  the other physical forces suggests that the
  universe actually has 11 dimensions (ten of space
  and one of time), seven of which are folded on
  themselves so that we cannot see them
• The idea of higher dimensions has motivated
  alternative cosmological models

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Key Words

• annihilation
• antimatter
• antiparticle
• antiproton
• cold dark matter
• cosmic light horizon
• density fluctuation
• deuterium bottleneck
• electroweak force
• elementary particle physics
• false vacuum
• flatness problem
• gluon
• grand unified theory (GUT)
• graviton
• Heisenberg uncertainty principle
• hot dark matter
• inflation
• inflationary epoch

• isotropy problem (horizon problem)
• Jeans length
• Kaluza-Klein theory
• Lamb shift
• M-theory
• nucleosynthesis
• pair production
• positron
• quantum electrodynamics
• quantum mechanics
• quark
• quark confinement
• spontaneous symmetry breaking
• strong force
• supergrand unified theory
• theory of everything (TOE)
• thermal equilibrium
• threshold temperature
• virtual pairs