j. goodman – may 2010 physics olympics neutrinos, dark matter and the cosmological constant the...
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J. Goodman – May 2010 Physics Olympics The Big Question in Cosmology What is the ultimate fate of the Universe?What is the ultimate fate of the Universe? –Will the Universe continue to expand forever? –Or will it collapse back on itself? We were told:We were told: –The answer depends on the energy density in the Universe – – mass and is the critical density. –If mass > 1 then the Universe is closed and it will collapse back –If mass < 1 then the Universe is open and it will expand forever stars = (1/2%) stars = (1/2%) –Is this the answer? Theory says > 1 < 1TRANSCRIPT
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Physics Olympics J. Goodman – May 2010
Neutrinos, Dark Matter and the Cosmological Constant
The Dark Side of the Universe
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Physics Olympics J. Goodman – May 2010
Outline
• The Cosmological Question – the fate of the Universe
• How do we know what the Universe is made of:– From atoms to quarks and leptons
• Why do we think there is Dark Matter• Data on the accelerating Universe
– Type Ia supernova– Cosmic Microwave Background
• Dark Energy• Neutrino Astronomy
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Physics Olympics J. Goodman – May 2010
The Big Question in Cosmology
• What is the ultimate fate of the Universe?– Will the Universe continue to expand forever?– Or will it collapse back on itself?
• We were told:
– The answer depends on the energy density in the Universe – W0
– W0= Wmass and W0=1 is the critical density.
– If Wmass > 1 then the Universe is closed and it will collapse back
– If Wmass < 1 then the Universe is open and it will expand forever
• Wstars= 0.005 (1/2%)
– Is this the answer?
• Theory says W0=1.0000 W > 1
W < 1
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Physics Olympics J. Goodman – May 2010
How do we know there really are atoms?
• Brownian Motion - Einstein
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Physics Olympics J. Goodman – May 2010
Seeing Atoms in the 21st Century
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Physics Olympics J. Goodman – May 2010
Seeing Atoms - Iron on Copper
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Physics Olympics J. Goodman – May 2010
Seeing into Atoms
• Atomic Spectra– We see spectral lines– The colors and the spacing of these lines tell us about
the structure of the atoms
E
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Physics Olympics J. Goodman – May 2010
Hydrogen Spectra
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Physics Olympics J. Goodman – May 2010
The structure of matter (cont.)
• All of this eventually gave a deeper understanding
Eventually this led toOur current picture of the atom and nucleus
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Physics Olympics J. Goodman – May 2010
What are fundamental particles?
• We keep finding smaller and smaller things
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Physics Olympics J. Goodman – May 2010
The search for fundamental particles
• Proton and electron– These were known to make up the atom
• The neutron was discovered• Free neutrons were found to decay
– They decayed into protons and electrons– But it looked like something was missing
• In 1930 Pauli postulated a unseen neutral particle
• In 1933 Fermi named it the “neutrino” (little neutron)
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Physics Olympics J. Goodman – May 2010
How do we know about things we can’t see?
Three Body Decay
Two Body Particle Decay
neutrino
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Physics Olympics J. Goodman – May 2010
Our current view of underlying structure of matter
• P is uud• N is udd• p+ is ud• k+ is us• and so
on…The Standard
Model
}Baryons
}Mesons
(nucleons)
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J. Goodman – August 2009Teachers as Scholars
Omega Minus Discovery
Particle Symbol Makeup Rest massMeV/c^2 B S Lifetime Decay Modes
Omega sss 1672 +1 -3 0.82x10-10
The omega-minus was produced by a K- p collision which produced the omega-minus and two kaons.
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J. Goodman – August 2009Teachers as Scholars
Quark Properties
Quark Symbol Spin Charge BaryonNumber S C B T Mass*
Up U 1/2 +2/3 1/3 0 0 0 0 360 MeV
Down D 1/2 -1/3 1/3 0 0 0 0 360 MeV
Charm C 1/2 +2/3 1/3 0 +1 0 0 1500 MeV
Strange S 1/2 -1/3 1/3 -1 0 0 0 540 MeV
Top T 1/2 +2/3 1/3 0 0 0 +1 174 GeV
Bottom B 1/2 -1/3 1/3 0 0 +1 0 5 GeV
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J. Goodman – August 2009Teachers as Scholars
• Baryons
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J. Goodman – August 2009Teachers as Scholars
• Baryons Mesons
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Table of Baryons
Particle Symbol Makeup Rest massMeV/c^2 Spin B S Lifetime
(seconds> Decay Modes
Proton p uud 938.3 1/2 +1 0 Stable ...
Neutron n ddu 939.6 1/2 +1 0 920
Lambda uds 1115.6 1/2 +1 -1 2.6x10-10
Sigma uus 1189.4 1/2 +1 -1 0.8x10-10
Sigma uds 1192.5 1/2 +1 -1 6x10-20
Sigma dds 1197.3 1/2 +1 -1 1.5x10-10
Delta uuu 1232 3/2 +1 0 0.6x10-23
Delta uud 1232 3/2 +1 0 0.6x10-23
Delta udd 1232 3/2 +1 0 0.6x10-23
Delta ddd 1232 3/2 +1 0 0.6x10-23
XiCascade uss 1315 1/2 +1 -2 2.9x10-10
XiCascade dss 1321 1/2 +1 -2 1.64x10-10
Omega sss 1672 3/2 +1 -3 0.82x10-10
Lmabda udc 2281 1/2 +1 0 2x10-13 ...
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J. Goodman – August 2009Teachers as Scholars
Lepton Properties
Particle Symbol Anti-particle
Rest massMeV/c2 L(e) L(muon) L(tau) Lifetime
(seconds)
Electron 0.511 +1 0 0 Stable
Neutrino(Electron) ~0(<7 x 10-6) +1 0 0 Stable
Muon 105.7 0 +1 0 2.20x10-6
Neutrino(Muon) ~0(<0.27) 0 +1 0 Stable
Tau 1777 0 0 +1 2.96x10-13
Neutrino(Tau) ~0(<31) 0 0 +1 Stable
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J. Goodman – August 2009Teachers as Scholars
SuperSymmetry
Name Spin Superpartner Spin
Graviton 2 Gravitino 3/2
Photon 1 Photino 1/2
Gluon 1 Gluino 1/2
W+,- 1 Wino+,- 1/2
Z0 1 Zino 1/2
Higgs 0 Higgsino 1/2
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Physics Olympics J. Goodman – May 2010
Measuring the Universe
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Physics Olympics J. Goodman – May 2010
Why do we think there is dark matter?
• Isn’t obvious that most of the matter in the Universe is in Stars?
Spiral Galaxy
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Physics Olympics J. Goodman – May 2010
Measuring the Matter in Galaxies
• In a gravitationally bound system out past most of the mass V ~ 1/r1/2
• We can look at the rotation curves of other galaxies– They should drop off
This is evidence for invisible matter or “Dark Matter”
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Physics Olympics J. Goodman – May 2010
Why do we think there is dark matter?
• There must be a large amount of unseen matter in the halo of galaxies– Maybe 20 times more than in the stars!– Our galaxy looks 30 kpc across but recent data
shows that it looks like it’s 200 kpc across
College Park
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Physics Olympics J. Goodman – May 2010
Lensing
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Physics Olympics J. Goodman – May 2010
Gravitational Lensing
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Physics Olympics J. Goodman – May 2010
Gravitational Lensing
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Physics Olympics J. Goodman – May 2010
Clusters produce distinctive tangential patterns
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Physics Olympics J. Goodman – May 2010
Measuring the energy in the Universe
• We can measure the mass of clusters of galaxies with gravitational lensing
• These measurements give Wmass ~0.3
• We also know (from the primordial deuterium abundance) that only a small fraction is nucleons
Wnucleons < ~0.04 Gravitational
lensing
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Physics Olympics J. Goodman – May 2010
Dark Matter
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Physics Olympics J. Goodman – May 2010
Dark Matter
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Physics Olympics J. Goodman – May 2010
Why do we care about neutrinos?
• Neutrinos – They only interact
weakly– If they have mass at all
– it is very small • They may be small, but
there sure are a lot of them!– 300 million per cubic meter
left over from the Big Bang– with even a small mass
they could be most of the mass in the Universe!
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Physics Olympics J. Goodman – May 2010
Facts about Neutrinos
• Neutrinos are only weakly interacting
• 40 billion neutrinos continuously hit every cm2 on earth from the Sun (24hrs/day)
• Interaction length is ~1 light-year of steel
• 1 out of 100 billion interact going through the Earth
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Physics Olympics J. Goodman – May 2010
What about neutrino mass?
• Could it be neutrinos?• How much neutrino mass would it take?
– Proton mass is 938 MeV– Electron mass is 511 KeV– Neutrino mass of 2eV would solve the galaxy
rotation problem – 20eV would close the Universe• Theories say it can’t be all neutrinos
– They have difficulty forming the kinds of structure observed. The structures they create are too large and form too late in the history of the universe
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Physics Olympics J. Goodman – May 2010
Does the neutrino have mass?
n
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Physics Olympics J. Goodman – May 2010
Detecting Neutrino Mass
• If neutrinos of one type transform to another type they must have mass:
• The rate at which they oscillate will tell us the mass difference between the neutrinos and their mixing
=
GeV
kmeVxe E
LmLP2
22 27.1ins2sin; nn
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Physics Olympics J. Goodman – May 2010
Neutrino Oscillations
n1 n2
=Electron n
Electron n
n1 n2
=Muon n
Muon n
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Physics Olympics J. Goodman – May 2010
Super-Kamiokande
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Physics Olympics J. Goodman – May 2010
How do we see neutrinos?
muonnm
m-
electronnee-
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Physics Olympics J. Goodman – May 2010
Cherenkov Radiation
Boat moves throughwater faster than wavespeed.
Bow wave (wake)
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Physics Olympics J. Goodman – May 2010
Cherenkov Radiation
Aircraft moves throughair faster than speed ofsound.
Sonic boom
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J. Goodman – Univ. of Maryland
Cherenkov Radiation
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Physics Olympics J. Goodman – May 2010
Cherenkov Radiation
When a charged particle moves throughtransparent media fasterthan speed of light in thatmedia.
Cherenkov radiation
Cone oflight
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Physics Olympics J. Goodman – May 2010
Cherenkov Radiation
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Physics Olympics J. Goodman – May 2010
Detecting neutrinos
Electron or
muon track
Cherenkov ring on the
wall
The pattern tells us the energy and type of particleWe can easily tell muons from electrons
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Physics Olympics J. Goodman – May 2010
A muon going through the detector
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Physics Olympics J. Goodman – May 2010
A muon going through the detector
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Physics Olympics J. Goodman – May 2010
A muon going through the detector
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Physics Olympics J. Goodman – May 2010
A muon going through the detector
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Physics Olympics J. Goodman – May 2010
A muon going through the detector
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Physics Olympics J. Goodman – May 2010
A muon going through the detector
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Physics Olympics J. Goodman – May 2010
Stopping Muon
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Physics Olympics J. Goodman – May 2010
Stopping Muon – Decay Electron
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Physics Olympics J. Goodman – May 2010
Atmospheric Oscillations
about 13,000 km
about 15
km
Neutrinos produced in
the atmosphere
We look for n transformations by looking at ns with different distances from production
SK
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Physics Olympics J. Goodman – May 2010
Telling particles apart
MuonElectron
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Physics Olympics J. Goodman – May 2010
Moderate Energy Sample
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Physics Olympics J. Goodman – May 2010
Neutrinos have mass
• Oscillations imply neutrinos have mass!• We can estimate that neutrino mass is
probably <0.2 eV – (we measure M2)• Neutrinos can’t make up much of the
dark matter – • But they can be as massive as all the
visible matter in the Universe!• ~ ½% of the closure density
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Physics Olympics J. Goodman – May 2010
Hubble Law
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Physics Olympics J. Goodman – May 2010
The expanding Universe
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Physics Olympics J. Goodman – May 2010
The expanding Universe
• The Universe is expanding
• Everything is moving away from everything
• Hubble’s law says the faster things are moving away the further they are away
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Physics Olympics J. Goodman – May 2010
Supernova
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Physics Olympics J. Goodman – May 2010
Actually Ia’s are “standardizable” candles
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Physics Olympics J. Goodman – May 2010
Supernova Cosmology Project
• Set out to directly measure the deceleration of the Universe
• Measure distance vs brightness of a standard candle (type Ia Supernova)
• The Universe seems to be accelerating!
• Doesn’t fit Hubble Law (at 99% c.l.)
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Physics Olympics J. Goodman – May 2010
The Cosmological Constant
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Physics Olympics J. Goodman – May 2010
Energy Density in the Universe
W0 may be made up of 2 parts a mass term and a “dark energy” L term (Cosmological Constant)
W0= Wmass + Wenergy
• Einstein invented L to keep the Universe static
• He later rejected it when he found out about Hubble expansion
• He called it his “biggest blunder”
L
mW0=1
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Physics Olympics J. Goodman – May 2010
Results of SN Cosmology Project
• The Universe is accelerating
• The data require a positive value of L “Cosmological Constant”
• If W0 =1 then they find
WL ~ 0.7 ± 0.1
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Physics Olympics J. Goodman – May 2010
Accelerating Universe
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Physics Olympics J. Goodman – May 2010
Accelerating Universe
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Physics Olympics J. Goodman – May 2010
Cosmic Microwave Background
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Physics Olympics J. Goodman – May 2010
Measuring the energy in the Universe
• Studying the Cosmic Microwave radiation looks back at the radiation from 400,000 years after the “Big Bang”.
• This gives a measure of W0
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Physics Olympics J. Goodman – May 2010
2002 Results
W0=1 Wnucleon
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Physics Olympics J. Goodman – May 2010
WMAP -2003
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Physics Olympics J. Goodman – May 2010
WMAP Results
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Physics Olympics J. Goodman – May 2010
WMAP - 2009
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Physics Olympics J. Goodman – May 2010
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Physics Olympics J. Goodman – May 2010
Density Fluctuations to Galaxies
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Physics Olympics J. Goodman – May 2010
Concordance model, aka LCDM
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Physics Olympics
Combining the Data 2010
J. Goodman – May 2010
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Physics Olympics J. Goodman – May 2010
Combining All Results
• Universe is 13.7 billion years old with a margin of error of close to 1%
• Expansion rate (Hubble constant) value: Ho= 71 km/sec/Mpc (with a margin of error of about 2%)
• Neutrinos only contribute as much matter as stars
• Content of the Universe: 4% Atoms, 23% Cold Dark Matter, 72% Dark energy.
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Physics Olympics J. Goodman – May 2010
What About Dark Matter?
• ~85% of the matter in the Universe is Dark Matter– At most a few % of the matter is baryons – Most people believe that the lightest SUSY particle is a
stable neutralino and is probably the dark matter– These are weakly interacting and heavy– LHC should be the answer…
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IceCube
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Physics Olympics
IceCube
J. Goodman – May 2010
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Physics Olympics J. Goodman – May 2010
χ
atm n
cosmic-ray μ’s
nm nm
χ
Sun
cosmic-ray
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Physics Olympics J. Goodman – May 2010
Conclusion
• Wtotal = 1.005 ± 0.006– The Universe is flat!
• The Universe is : ~1/2% Stars
~1/2% Neutrinos ~27% Dark Matter
(only 4% is ordinary baryonic matter)
~72% Dark Energy
• We can see ~1/2%• We can measure ~1/2%• We can see the effect of
~27% (but don’t know what most of it is)
• And we are pretty much clueless about the other 3/4 of the Universe
There is still a lot of Physics to learn!
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Physics Olympics J. Goodman – May 2010