our universe and its dark side - · pdf fileour universe and its dark side david morrissey...
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Our Universeand its Dark Side
David Morrissey
RASC Lecture, October 14, 2011
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Cosmology
• Big questions about the Universe:
1. What is its structure over very large distances?
2. How did it evolve over time?
3. Can we explain it using the physics we know?
• The third question is the most ambitious.
“Physics we know” comes from experiments on Earth.
Will it still work over much larger astronomical distances?
• Short Answer: yes, but we need some “dark” stuff.
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Looking Around,
from Near to Far
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Stars
• We are orbiting the sun.
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Galaxies
• Stars tend to collect into galaxies.
Ours is the Milky Way.
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Galaxy Clusters and Superclusters
• Galaxies collect in clusters and superclusters.
Ours is the Local Group and the Virgo Supercluster.
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And Beyond . . .
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Making Sense of It All
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Cosmology = Astronomy Zoomed Way Out
• Two Main Observations:
1. Everything is the same everywhere (on average).
2. Empty space isn’t empty – it has a faint amount of light.
• We can use these facts, together with known physics,
to (mostly) reconstruct the history of the Universe.
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Important Observation #1
• The universe is the same in all directions, on average:
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Important Observation #2
• Empty “outer space” is not quite empty.
It is filled a very faint glow of light.
• This Cosmic Microwave Background (CMB)
has a temperature of T ≃ 2.73K.
(Room temperature is about 293K, freezing is 273K.)
• The CMB is extremely uniform: ∆T/T ≃ 1/10000.
These variations contain a lot of information.
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• Cosmic Microwave Background (CMB).
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• Temperature Fluctuations
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What Gravity has to Say About This
• Gravity is this only force that matters over
astronomical and cosmological distances.
• theory of gravity ↔ General Relativity [Einstein 1915]
gravity force ↔ warping of space and time
amount of warping ↔ amount of energy
• Look for gravity solutions that:
i) describe a spacetime that is the same everywhere
ii) contain a smooth density of matter and energy
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• Prediction: spacetime is expanding.
Expansion is described by a scale factor a(t):
t1: free particles A and B are separated by distance L.
t2: free particles A and B are separated by a(t2)a(t1)
L > L.
• Non-free particles DO NOT move apart!
(e.g. rulers don’t get longer)
L
a2_a1
L
t
t
1
2
Acme Ruler Company
Acme Ruler Company
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• This is precisely what we see – Hubble Expansion.
Distant galaxies are moving away from us.
(recession speed) ≃ H × (distance), H =a
a> 0
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The Big Bang [Alpher,Bethe,Gamow ’1947]
• Remember all that T = 2.73K CMB light?
As the universe expands it cools off.
• Going back in time, the universe must have been
much hotter in the past.
• T → ∞ as t → 0!
Big Bang!
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High Temperatures and Elementary Particles
• The early Universe was very very hot.
• At high temperatures, matter gets ripped apart
into its basic building blocks.
⇒ elementary particle physics
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Elementary Particles and Fundamental Forces
νe νν0
+−
γ
d s b
τ
c t
µ
µ τh
u
Fermions Bosons
Z
W
e
g
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In Stuffed Toy Form
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Predictions for the History of the Universe
• t = 10−10 s: hot soup of elementary particles
• t = 10−6 s: quarks bind to form protons and neutrons
• t = 1 s−1min: protons and neutrons bind to form nuclei
• t = 10000 yrs: dust starts to clump gravitationally
• t = 100000 yrs: electrons and nuclei bind to form atoms
• t = 100million yrs: clumps of dust ignite to make stars
• t = 13.7 billion yrs: today
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Confronting Data
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Does our Cosmological Model Work?
• Almost:
– predicted light element abundances match data
– leftover light from the big bang is seen as the CMB
– stars and galaxies form as we expect them to
• But not quite:
– there seems to be more matter than we can account for
– the expansion of the Universe today is accelerating
• Two new ingredients are needed:
Dark Matter and Dark Energy .
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Cosmic Microwave Background Radiation
• At t = 100000 yrs, electrons and nuclei bind into atoms.
• With no free electric charges, light travels unimpeded.
• This light is what we see today as the T = 2.73K
cosmic microwave background (CMB) light.
Surface of Last Scattering
Us
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• Cosmic Microwave Background (CMB).
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• Variations in the Cosmic Microwave Background (CMB)
temperature contain a lot of information.∗
* 2006 Nobel Prize to Mather and Smoot for finding these variations.
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• Height and location of the peaks and troughs depend on
the energy content and the geometry of the Universe.
ΩΛ
0.2 0.4 0.6 0.8
20
40
60
80
100
∆ T(µ
K)
Ωtot
0.2 0.4 0.6 0.8 1.0
Ωbh2
10
0.02 0.04 0.06
100 1000
20
40
60
80
100
l
∆ T(µ
K)
10 100 1000
l
Ωmh2
0.1 0.2 0.3 0.4 0.5
(a) Curvature (b) Dark Energy
(c) Baryons (d) Matter
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CMB Results
• The Universe is spatially flat.
• Energy Content:
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Dark Matter
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Missing Matter: Gravitational Lensing
• Gravitational Lensing: light is bent by gravity.
(Amount of Bending) ∼ (Amount of Matter)
• Much more matter than is visible!
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Missing Matter: Galactic Structure
• We need hidden matter to explain the structure
of galactic superclusters.
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• Dark matter is pulled together into clumps by gravity.
Visible matter gets sucked in and forms stars, galaxies, . . .
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Missing Matter: Galactic Rotation
• Many galaxies rotate.
Rotation Rate ↔ Amount of Matter they Contain
• Hidden matter is needed to explain galactic rotation.
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Missing Matter = Dark Matter
• Hidden cosmological matter is called Dark Matter (DM).
• None of the known particles can be the DM.
They all give off too much light.
• A DM particle needs to be heavy, stable, and neutral.
• DM Hunting:
– Create DM in particle colliders (LHC).
– Look for DM scattering off sensitive detectors.
– Search for DM effects in our galaxy.
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• We might be able to create DM in particle collisions.
e.g. CERN LHC: high-energy proton-proton collisions
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• DM could also be observed directly.
Look for unexplained particle scattering.
Nucleus
DM
Detector
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Dark Energy
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Cosmic Acceleration
• Recent expansion of the Universe can be measured
by studying Type IA supernova.
• Distance to a Type IA supernova can be determined
from its brightness and its characteristic light curve.
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• Light emitted by a supernova at time time t1
observed at a later time t2 is shifted in wavelength:
(observed wavelength) =a(t2)
a(t1)× (emitted wavelength) .
• Colour → Wavelength
Brightness → Distance → Time of Emission (t1)
• Measuring many supernova allows us to determine a(t).
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• Astronomers did just this.∗
• Result: the expansion rate is accelerating.
* 2011 Nobel Prize to Perlmutter, Reiss, and Schmidt
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Dark Energy
• Accelerated expansion requires dark energy.
• Regular matter does not work: it is diluted by the expansion.
• Dark Energy = intrinsic energy of empty space
It does not dilute as a result of spacetime expansion.
• Where does it come from?
Best Guess: quantum mechanical effects on empty space.
• New observations will give us more information.
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Summary
• Physics on the Earth seems to work in the Cosmos!
• Ingredients: particle physics and general relativity .
– Start with a hot plasma of elementary particles
– Expand and cool
– Form nucleons, nuclei, atoms, stars, galaxies, . . .
• But what is the Dark Matter and the Dark Energy?
More experiments and observations are underway . . .
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Extra Slides
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Hot Soup: t ∼ 10−10 s
• Start with a hot soup of elementary particles at T ∼ 1014K.
– free quarks and gluons
– electrons and photons
– muons, taus, neutrinos
– W±, Z0, Higgs, . . .
• The soup cools as the Universe expands.
Unstable particles decay away and disappear.
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Protons and Neutrons: t ≃ 10−6 s
• Protons and neutrons form when T falls below 1012K.
Proton = p = u+ u+ d
Neutron = n = u+ d+ d
• Why? Binding Strength ∼ mpc2 ∼ mnc2 ∼ 1012K.
T > 1012K: plasma collisions rip nucleons apart
T < 1012K: plasma collisions don’t have enough energy
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Light Nuclei: t ≃ 1 s – 1min
• At T > 109K (t < 1 s) we have:
p+ e− ↔ n+ νe, (mn −mp = 1.2MeV)
• For T < 109K the reverse reaction is more likely.
The reaction “turns off” when T ≃ 0.3× 109K with
Nn
Np≃
1
7.
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• At T < 0.1MeV, some light nuclei start to form:
p+ n → D + γ
p+D → 32He+ γ
n+ 32He → 4
2He+ γ
. . ..
n
p n
p
np
p
n
n p
np
p
D
He
He
.
4
3
2
2
.
• We can predict element abundances from particle physics!
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• Calculations agree well with observations:
• Only light (A . 7) nuclei are produced this way
due to small temperatures and densities.
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Atoms: t ≃ 1010s ≃ 1000 yr
• Hydrogen atom:
Binding Strength = 13.6 eV
⇒ for T > 13.6eV we only have ions and free electrons.
• For T < 13.6 eV, electrons and nuclei bind into atoms:
p+ e− → H + γ
• Nearly all free charges are bound by T ≃ 0.3 eV (t ≃ 1012 s).
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• With no free charges, photons nothing to scatter with.
⇒ light travels unimpeded
⇒ universe becomes transparent
• These photons are what we see today as the T ≃ 2.73K
cosmic microwave background (CMB) light.
Surface of Last Scattering
Us
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The Cosmic Microwave Background (CMB)
• The CMB is a snapshot of the universe at recombination.
• It is almost completely uniform: ∆T/T ≃ 10−4
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Structure Formation: t > 1010 s ≃ 1000 yrs
• CMB spots represent local density variations.
• These grow with time, and eventually become
unstable to gravitational collapse at t ≃ 1010s.
• Gravity pulls matter together into clumps of dust
that eventually become galaxies, stars, planets, . . .
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Star Formation: t > 1015s ≃ 100 million yrs
• Clumps of dust get pulled together by gravity at t ≃ 1015 s.
As they condense, they heat up.
• Thermal pressure eventually balances out gravity when
Tdust ≃ 108K ≃ 0.01MeV,
hot enough to ignite nuclear fusion and make a star!
• Stars evolve over their lifetime to make heavier elements.
We can predict their abundances as well!
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• ttoday ≃ 13.7 billion yrs
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H Burning: Main Sequence Stars
• H burning is the first process to take place:
p+ p → D + e+ + νe
p+D →32He+ γ
32He+ 3
2He →42He+ p+ p
• Net result: 6p → 42He+2p. (Other processes too.)
• Energy released by H burning provides thermal pressure
that supports the start from gravitational collapse.
• Star supported only by H burning = “main sequence”.
The sun is a familiar example of this.
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He Burning and Beyond: Giants
• When H is used up: – gravity compresses the core more
– the core heats up
– He burning starts
• He burning: 42He+ 4
2He+ 42He → 12
6 C, 42He+ 12
6 C → 168 O
• When 42He is used up, C and O burning kicks in.
• (Red) Giant Star
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• 2010Ne, 24
11Na, 2412Mg burning next.
• 2814Si burning next
• This chain stops when the core becomes 5628Fe.
5628Fe is the lowest energy nuclear state.
⇒ no more energy can be obtained from nuclear fusion
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• So what next?
• Big stars with M & 10M⊙ blow up – supernova!
• Smaller stars might never get to the 5628Fe core stage.
• White dwarf = star supported by electron degeneracy.
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Supernova!
• Big stars with a 5628Fe core can no longer support
themselves against gravity.
• The core collapses creating a huge pressure.
Pure neutron matter then becomes energetically favourable.
p → n+ e+νe
• Neutron degeneracy pressure stops the core collapse.
• The core “bounces” sending off a shock wave
and that blows away the outer layers of the star.
→ Supernova!!!
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• Heavy elements are produced in the outgoing
neutron-rich shock wave via the r-process.
• These drift off, and are incorporated into new stars.