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Today: “Nucleosynthesis… another phase change in early universe… and why is the Universe so Flat?”. HW for next time: Onion, “the nucleus and forces of nature” chapters 3 & 4 reminder: use the Glossary Session 7: 2/6/07 ? min. - PowerPoint PPT Presentation
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Today: “Nucleosynthesis… another phase change in early universe…
and why is the Universe so Flat?”
HW for next time:
Onion, “the nucleus and forces of nature”
chapters 3 & 4
reminder: use the Glossary
Session 7: 2/6/07 ? min
geometry of universe:
determined by total density of matter & energy
Density = Critical
Density > Critical
Density < Critical
why is the density ~ critical…i.e. why is our universe so“flat?”
Inflation flattens overall geometry like blowing up a balloon,
overall density of matter plus energy becomes almost critical
…during the first 3 minutes, Big Bang nucleosynthesis created
deuterium (d), 3He, 4He, traces of Li…but nothing else
at t ~1 minute, universe cooled to temperature T ~ 1MeV, nuclear energies
E = kT, 1 MeV ~ 1010 °K
1/40 eV ~10,000 °K
too cool for n↔p equilibrium since mn > mp by 1.3 MeV,
mn ~ mp = 1 GeV = 1000 MeV
so neutrons weakly decay n → p e beta decay
between 1 and 3 minutes,
temperature high enough to fuse n + p → d, then d + t → He t=tritium=3H
not too high to dissociate weakly-bound d 2.2 MeV binding energy
nor to destroy very stable 4He (=α) 24 MeV binding energy
at t = 1 min, Big Bang predicts protons:neutrons = 7:1
after 3 minutes, universe too cool to fuse a neutron and proton to deuterium,
but all neutrons already bound up in helium! 4He2 = α= 2 protons + 2 neutrons
(read Steve Weinberg’s “The First Three Minutes”)
In hot primordial plasma, protons and neutrons combine making ultra-stable, long-lasting helium
but universe only hot enough up to ~ 3 minutes of age
one of the reaction chains… JET, next ITER
Big Bang theory prediction: 75% H, 25% He (12/16 vs 4/16 by mass) Matches observations of primordial gases in star forming regions
Big Bang theory: correctly predicts trace abundances of elements 2H = d, 3He, Li?
(will discuss horizontal axis when we discuss at dark matter)
But, can you observing the Big Bang for yourself? the snow on the TV…darkness of the night sky…evidence for Big Bang
first Kepler, thenOlbers’ Paradox
If universe were
1) infinite
2) unchanging
3) everywhere the same
stars would cover the night sky
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
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
…now, in summary
a brief history of the universe
as motivation for our study of particle physics
Four known forces in universe:
Strong Force Electromagnetism
Weak Force
Gravity
Do forces unify at high temperatures?
Yes!Fermilab & Cern
Proton Decay (GUT?)
Who knows?(String Theory)
Planck Era
Before Planck time (~10-43 sec)
No theory of quantum gravity
GUT Era
Lasts from Planck time (~10-43 sec) to end of GUT force (~10-38 sec)
Electroweak Era
Lasts from end of GUT force (~10-38 sec) to end of electroweak force (~10-10 sec)
Quark Era
Amounts of matter and antimatter nearly equal
(Roughly 1 extra proton for every 109 proton-antiproton pairs!)
Era of Nucleo-synthesis
Begins when matter annihilates remaining antimatter at ~ 0.001 sec
Nuclei begin to fuse
Era of Nuclei
Helium nuclei form at age ~ 3 minutes
Universe has become too cool to blast helium apart
Era of Atoms
Atoms form at age ~ 380,000 years
Background radiation released
Era of Galaxies
Galaxies form at age ~ 1 billion years
RESERVE
PHOTONS DECOUPLING
from H & He atoms once formed
interactive
History of Universewith black body spectra red shifted
for each era
interactive
Light from disconnected regionscoupled after inflation
interactive
The early universe must have been extremely hot and dense