july 27, 2004 part i: expanding universe part ii: what’s the matter in the universe? july 27, 2004
TRANSCRIPT
July 27, 2004
Part I: Expanding Universe Part II: What’s the matter in the
Universe?
July 27, 2004
July 27, 2004
Big Bang?
• Did the Big Bang really happen?
• Is the Universe really expanding?
• Did the BB include inflation?
• How can we find out?
July 27, 2004
Debate preparation
• Big bang vs. steady state Universe
July 27, 2004
Debate and Debrief
• Debrief slides follow
July 27, 2004
Standard Big Bang Cosmology
• Sometime in the distant past there was nothing – space and time did not exist
• Vacuum fluctuations created a singularity that was very hot and dense
• The Universe expanded from this singularity• As it expanded, it cooled
– Photons became quarks– Quarks became neutrons and protons– Neutrons and protons made atoms– Atoms clumped together to make stars and
galaxies
July 27, 2004
Standard Big Bang Cosmology
• Top three reasons to believe standard big bang cosmology
1. Hubble Expansion
2. Big Bang Nucleosynthesis
3. Cosmic Microwave Background
Big Bang by Physics Chanteuse Lynda Williams
July 27, 2004
Cepheid variables and Nebulae
• In 1923, Hubble used new Mt. Wilson 100 inch telescope to observe Cepheid variables in the nearby “nebula” Andromeda. He recognized that the fuzzy patches called nebulae were actually distant galaxies, outside of our own Milky Way
L =K P1.3
This relation was calibrated by Hertzsprung and Shapley
July 27, 2004
Hubble LawThe Hubble constant
Ho = 558 km s -1 Mpc -1
is the slope of these graphs
Compared to modern measurements, Hubble’s
results were off by a factor of ten!
July 27, 2004
Recall Doppler Shift
Redshift z is a non-relativistic approximation that relates the Doppler shift to the velocity of the object
Redshift is determined by comparing laboratory wavelength to observed wavelength
=
vc
=z =
July 27, 2004
Hubble Law• v = Ho d = cz where
– v = velocity from spectral line measurements– d = distance to object– Ho = Hubble constant in km s-1 Mpc -1 – z is the redshift
Space between the galaxies expands while galaxies stay the same size
July 27, 2004
Expanding Universe
• Expanding Universe of Dots– Why it always looks as though you are at
the center of the expanding universe
• Expanding Universe of Students– The farther things are, the faster they are
moving away
July 27, 2004
Doppler shifting spectral lines
• When a star or galaxy is moving, its spectral lines are Doppler shifted by = obs – lab
• The redshift Z = /lab
• The velocity of the star or galaxy is found from the redshift using v = ZAVG c
H and K lines
July 27, 2004
Hubble constant
• Contemporary Lab Experiences in Astronomy Project CLEA
• You will plot the velocities (km/sec) vs. the distances (Mpc) that you obtain from a sample of galaxies
• The slope of this line is known as the Hubble constant – it is given in km/sec/Mpc
Ho = v/D
July 27, 2004
Contemporary Lab Experiences in Astronomy Project CLEA
• Read through “The Hubble Redshift Distance Relation” student manual
• This manual will walk you through the steps to running the lab.
• Break up into 6 groups of four
July 27, 2004
The age of the Universe
• What is the relationship to the Hubble constant and the age of the Universe?
• Recall Ho = v/D• What are the units?
– D must be in km – V must be in km/sec
• What does this give us?• How do we convert this number into years?
July 27, 2004
Big Bang Timeline
We are hereBig Bang Nucleosynthesis
July 27, 2004
Big Bang Nucleosynthesis• Light elements (namely deuterium, helium, and
lithium) were produced in the first few minutes after the Big BangThe predicted abundance of light elements heavier than hydrogen, as a function of the density of matter in the universe (where 1 is critical)
Note the steep dependence of deuterium on critical density.
Goal is to find a density that explains all the abundances that are measured (blue line)
July 27, 2004
Big Bang Nucleosynthesis
• Heavier elements than 4He are produced in the stars and through supernovae
• However, enough helium and deuterium cannot be produced in stars to match what is observed – in fact, stars destroy deuterium in their cores, which are too hot for deuterium to survive.
• So all the deuterium we see must have been made around three minutes after the big bang, when T~109 K
• BBN predicts that 25% of the matter in the Universe should be helium, and about 0.001% should be deterium, which is what we see.
• BBN also predicts the correct amounts of 3He and 7Li
July 27, 2004
Big Bang Timeline
We are hereCosmic
Microwave Background
July 27, 2004
Cosmic Microwave Background
• Discovered in 1965 by Arno Penzias and Robert Wilson who were working at Bell Labs
• Clinched the hot big bang theory
Excess noise in horned antennae was not due to pigeon dung!
July 27, 2004
• Photons in CMB come from the time in the Universe where they stop interacting with matter and travel freely through space
• CMB photons emanate from a cosmic photosphere – like the surface of the Sun – except that we inside it looking out
• The cosmic photosphere has a temperature which characterizes the radiation that is emitted
• It has cooled since it was formed by more than 1000 to 2.73 degrees K
CMB
July 27, 2004
COBE data• “Wrinkles on the face of God”
July 27, 2004
COBE data• Fluctuations in CMB are at the level of one part in 100,000
Blue spots mean greater density
Red spots mean lesser density
(in the early Universe)
July 27, 2004
• Insert WMAP BE Video
July 27, 2004
WMAP vs. COBE
• The WMAP image brings the COBE picture into sharp focus.
movie
July 27, 2004
Universe’s Baby Pictures
Red is warmer
Blue is cooler Credit:
NASA/WMAP
July 27, 2004
Compare MAPs at other wavelengths
• Visible to microwave galaxy images
• Compare the dynamic range
movie
July 27, 2004
WMAP measures geometry
July 27, 2004
Another way to measure geometry
See how parallel laser light beams fired by the space slug are affected by the geometry of space
July 27, 2004
Big Bang Timeline
We are hereInflation
July 27, 2004
What is inflation?• Inflation refers to a class of cosmological
models in which the Universe exponentially increased in size by about 1043 between about 10-35 and 10-32 s after the Big Bang (It has since expanded by another 1026)
• Inflation is a modification of standard Big Bang cosmology
• It was originated by Alan Guth in 1979 and since modified by Andreas Albrecht, Paul Steinhardt and Andre Linde (among others)
July 27, 2004
Why believe in inflation?• Inflation is a prediction of grand unified
theories in particle physics that was applied to cosmology – it was not just invented to solve problems in cosmology
• It provides the solution to two long standing problems with standard Big Bang theory
– Horizon problem
– Flatness problem
Alan Guth
July 27, 2004
WMAP supports inflation
• Inflation - a VERY rapid expansion in the first 10-35 s of the Universe – predicts:– That the density of the universe is close to the
critical density, and thus the geometry of the universe is flat.
– That the fluctuations in the primordial density in the early universe had the same amplitude on all physical scales.
– That there should be, on average, equal numbers of hot and cold spots in the fluctuations of the cosmic microwave background temperature.
• WMAP sees a geometrically flat Universe
July 27, 2004
Horizon Problem• The Universe looks the same everywhere in
the sky that we look, yet there has not been enough time since the Big Bang for light to travel between two points on opposite horizons
• This remains true even if we extrapolate the traditional big bang expansion back to the very beginning
• So, how did the opposite horizons turn out the same (e.g., the CMBR temperature)?
July 27, 2004
No inflation• At t=10-35 s, the Universe expands from
about 1 cm to what we see today
• 1 cm is much larger than the horizon, which at that time was 3 x 10-25 cm
July 27, 2004
With inflation
• Space expands from 3 x 10-25 cm to much bigger than the Universe we see today
July 27, 2004
Flatness Problem• Why does the Universe seem to be flat?• Inflation flattens out spacetime the same way
that blowing up a balloon flattens the surface• Since the Universe is far bigger than we can
see, the part of it that we can see looks flat
July 27, 2004
Lunch
• What’s the matter in the universe?
• Why are there so many more particles than anti-particles?
• How do we know?
July 27, 2004
Big Bang Timeline
We are here
This lecture
July 27, 2004
Probing structure of matter
• Given: a large wooden board, a mystery shape and marbles
• Try to identify the shape that is hiding under the wooden board. You can only roll marbles against the hidden object and observe the deflected paths that the marbles take. Take at least five minutes to "observe" a shape. Then do a second shape.
• Place a piece of paper under the board for sketching the paths of the marbles. Then analyze this information to determine the object's actual shape.
July 27, 2004
Analysis
• Black vertical line shows path of incoming marble
• Red line shows path of outgoing marble
• Green dotted line bisects the angle made by the incoming and outgoing lines
• Reflecting surface is perpendicular to bisecting line
July 27, 2004
Questions
• Draw a small picture of each shape you studied in your binder.
• Can you tell the size of the object as well as its shape?
• How could you find out whether the shape has features that are small compared to the size of your marbles?
• Without looking, how can you be sure of your conclusions?
July 27, 2004
Atomic Structure
• Rutherford shot alpha-particles (Helium nuclei) at a thin gold foil. He found that most went right through. However, some were deflected, and a percentage of those bounced right back at him! He said that “it was like firing a cannonball at tissue paper, and having it ricochet off!”
• Can you see how he concluded that the nucleus was a hard small sphere, and that most of the atom was empty space? (As opposed to a plum pudding?)
July 27, 2004
Atomic Particles
• Atoms are made of protons, neutrons and electrons
• 99.999999999999% of the atom is empty space• Electrons have locations
described by probability functions
• Nuclei have protons and neutrons
nucleus
mp = 1836 me
July 27, 2004
Leptons
• An electron is the most common example of a lepton – particles which appear pointlike
• Neutrinos are also leptons• There are 3 generations of leptons, each has
a massive particle and an associated neutrino• Each lepton also has an anti-lepton (for
example the electron and positron)• Heavier leptons decay into lighter leptons
plus neutrinos (but lepton number must be conserved in these decays)
July 27, 2004
Types of Leptons
Lepton Charge
Mass (GeV/c2)
Electron neutrino
0 0
Electron -1 0.000511
Muon neutrino
0 0
Muon -1 0.106
Tau neutrino
0 0
Tau -1 175
July 27, 2004
Quarks
• Experiments have shown that protons and neutrons are made of smaller particles
• We call them “quarks”, a phrase coined by Murray Gellman after James Joyce’s “three quarks for Muster Mark”
• Every quark has an anti-quark
Modern picture of atom
July 27, 2004
Atomic sizes• Atoms are about 10-10 m• Nuclei are about 10-14 m• Protons are about 10-15 m• The size of electrons and
quarks has not been measured, but they are at least 1000 times smaller than a proton
July 27, 2004
Types of QuarksFlavor Charge Mass
(GeV/c2)
Up 2/3 0.003
Down -1/3 0.006
Charm 2/3 1.3
Strange -1/3 0.1
Top 2/3 175
Bottom -1/3 4.3
• Quarks come in three generations
• All normal matter is made of the lightest 2 quarks
July 27, 2004
Quarks
• Physics Chanteuse
Up, down, charm, strange, top and bottomThe world is made up of quarks and leptons…
Quark Sing-A-long
July 27, 2004
Combining Quarks
• Particles made of quarks are called hadrons
• 3 quarks can combine to make a baryon (examples are protons and neutrons)
• A quark and an anti-quark can combine to make a meson (examples are muons and kaons)
proton
meson
• Fractional quark electromagnetic charges add to integers in all hadrons
July 27, 2004
Color charges
• Each quark has a color charge and each anti-quark has an anti-color charge
• Particles made of quarks are color neutral, either R+B+G or color + anti-color
Quarks are continually changing their colors – they are not one color
July 27, 2004
Gluon exchange• Quarks exchange gluons within a nucleon
movie
July 27, 2004
Atomic Forces
• Electrons are bound to nucleus by Coulomb (electromagnetic) force
• Protons in nucleus are held together by residual strong nuclear force
• Neutrons can beta-decay into protons by weak nuclear force, emitting an electron and an anti-neutrino
F = k q1 q2
r2
n = p + e +
July 27, 2004
Fundamental Forces
• Gravity and the electromagnetic forces both have infinite range but gravity is 1036 times weaker at a given distance
• The strong and weak forces are both short range forces (<10-14 m)
• The weak force is 10-8 times weaker than the strong force within a nucleus
July 27, 2004
Force Carriers
• Each force has a particle which carries the force
• Photons carry the electromagnetic force between charged particles
• Gluons carry the strong force between color charged quarks
July 27, 2004
Force Carriers
• Separating two quarks creates more quarks as energy from the color-force field increases until it is enough to form 2 new quarks
• Weak force is carried by W and Z particles; heavier quarks and leptons decay into lighter ones by changing flavor
July 27, 2004
Unifying Forces
• Weak and electromagnetic forces have been unified into the “electroweak” force – They have equal strength at 10-18 m– Weak force is so much weaker at larger distances
because the W and Z particles are massive and the photon is massless
• Attempts to unify the strong force with the electroweak force are called “Grand Unified Theories”• There is no accepted GUT
July 27, 2004
Gravity• Gravity may be carried by the graviton – it
has not yet been detected • Gravity is not relevant on the sub-atomic
scale because it is so weak• Scientists are trying to find a “Theory of
Everything” which can connect General Relativity (the current theory of gravity) to the other 3 forces
• There is no accepted Theory of Everything (TOE)• Superstrings are the basis of a class of TOEs
July 27, 2004
Force Summary
July 27, 2004
Standard Model
• 6 quarks (and 6 anti-quarks)• 6 leptons (and 6 anti-leptons)• 4 forces• Force carriers (, W+, W-, Zo, 8 gluons, graviton)
July 27, 2004
Some questions
• Do free quarks exist? Did they ever?• Why do we observe matter and almost no antimatter if
we believe there is a symmetry between the two in the universe?
• Why can't the Standard Model predict a particle's mass? • Are quarks and leptons actually fundamental, or made
up of even more fundamental particles? • Why are there exactly three generations of quarks and
leptons? • How does gravity fit into all of this?
July 27, 2004
Particle Accelerators
• The Standard Model of particle physics has been tested by many experiments performed in particle accelerators
• Accelerators come in two types – hadron and lepton• Heavier particles can be made by colliding lighter
particles that have added kinetic energy (because E=mc2)
• Detectors are used to record the shower of new particles that results from the collision of the particle/anti-particle beams
July 27, 2004
Particle Accelerators-SLAC
• 2 mile long accelerator which can make up to 50 GeV electrons and positrons
• Now being used as an asymmetric B-meson factory, making Bs and anti-Bs out of 9 GeV electrons and 3.1 GeV positrons
July 27, 2004
SLAC B-factory• Goal is to understand the
imbalance between matter and anti-matter in the Universe
• 1 out of every billion matter particles must have survived annihilation
• Decay rates of Bs and anti-Bs should be different
• Explanation goes beyond the standard model
July 27, 2004
FermiLab
• 5 accelerators which collide protons and
anti-protons at 2 TeV
Colliding Detector at Fermilab (CDF) D0
July 27, 2004
Picturing Particles Activity
• Analyze the events that are seen in different chambers of a detector
• Determine the particles that could have made these tracks
• Remember that positively charged particles curve opposite to negatively charged particles due to the magnet in the detector
• Muons are not stopped by any of the layers – they travel through the entire detector
• Electrons (positrons) and photons are stopped in the electromagnetic calorimeter layer
• Hadrons are stopped in the hadron calorimeter
July 27, 2004
Figures for activity
July 27, 2004
Break
• So now that we know some particle physics, what does this have to do with the Universe on large scales?
July 27, 2004
Unified Forces• The 4 forces are all unified (and therefore
symmetric) at the beginning of the Universe.
beginning of the Universe
inflation
July 27, 2004
Broken Symmetry
• At high T, the Universe is in a symmetrical state, with a unique point of minimum energy
• As the Universe cools, there are many possible final states – but only one is chosen when the symmetry breaks
Which glass goes with which
place setting?
July 27, 2004
Phase transitions• The unified (symmetric) state of the very early
Universe is a state of negative energy called the false vacuum
• A phase transition turns the false vacuum into the true vacuum and provides the surge of energy that drives inflation – similar to the energy released when water freezes into ice
• This occurs when the strong nuclear force splits off from the electroweak force
• During inflation, spacetime itself expands faster than the speed of light and small density fluctuations are created to seed structure formation
July 27, 2004
Child Universes
• As the false vacuum turns into true vacuum, particles are created in “child universes”
• The child universe disconnects from the original space
True vacuum
False vacuum
Child Universe
Observers in the parent universe see a black hole form!
July 27, 2004
Multiverses
• Universe was originally defined to include everything
• However, with inflation, the possibility exists that our “child universe” is only one of many such regions that could have formed
• The other universes could have very different physical conditions as a result of different ways that the unified symmetry was broken
• New universes may be forming with each gamma-ray burst that makes a black hole!
July 27, 2004
A Humbling Thought• Not only do we not occupy a preferred place
in our Universe, we don’t occupy any preferred universe in the Multiverse!
July 27, 2004
Reflection and Debrief
• Now what do we know?
• What are the big ideas here?
• What do our students need to know?
• Is there anything else we need to know?
• Misconceptions
(take notes)
July 27, 2004
Reflection and Debrief
• What are some of the effective ways to teaching these topics?
• Standards???
(take notes)
July 27, 2004
Web Resources The Particle Adventure http://particleadventure.org/
SLAC http://www.slac.stanford.edu
FermiLab http://www.fnal.gov/pub/tour.html
Virtual Space time travel machine http://www.lactamme.polytechnique.fr/Mosaic/descripteurs/demo_14.html
CERN http://public.web.cern.ch/Public/
Particle Physics Education Sites http://particleadventure.org/particleadventure/other/othersites.html
July 27, 2004
Web Resources• Cosmic Background Explorer
http://space.gsfc.nasa.gov/astro/cobe/cobe_home.html• George Smoot’s group pages http://aether.lbl.gov/
• University of Washington Curvature of Space http://www.astro.washington.edu/labs/clearinghouse/labs/Curvature/curvature.html
• Ned Wright’s Cosmology Tutorial http://www.astro.ucla.edu/~wright/cosmolog.htm
• James Schombert Lectures http://zebu.uoregon.edu/~js/21st_century_science/lectures/lec24.html
• CLEA Astronomy Laboratories http://www.gettysburg.edu/academics/physics/clea/CLEAsoft.overview.html
July 27, 2004
Web Resources
Ned Wright’s CMBR pages http://www.astro.ucla.edu/~wright/CMB-DT.html
Bell Labs Cosmology Archives http://www.bell-labs.com/project/feature/archives/cosmology/
Physics Web quintessence http://physicsweb.org/article/world/13/11/8Big Bang Cosmology Primer http://cosmology.berkeley.edu/Education/IUP/Big_Bang_Primer.html
Martin White’s Cosmology Pages http://astron.berkeley.edu/~mwhite/darkmatter/bbn.html
July 27, 2004
More Resources
Inflationary Universe by Alan Guth (Perseus) A Short History of the Universe by Joseph Silk (Scientific American Library) Before the Beginning by Martin Rees (Perseus) Inflation for Beginners (John Gribbin) http://www.biols.susx.ac.uk/Home/John_Gribbin/cosmo.htm
Ned Wright’s Cosmology Tutorial http://www.astro.ucla.edu/~wright/cosmolog.htm
July 27, 2004
Web Resources
Thanks also to Dr. Gordon Spear for providing his Hubble Law Lab spreadsheet!
July 27, 2004
Web Resources (expanding universe)
• Astronomy picture of the Day http://antwrp.gsfc.nasa.gov/apod/astropix.html
• Imagine the Universe http://imagine.gsfc.nasa.gov
• Ned Wright’s ABCs of Distance http://www.astro.ucla.edu/~wright/distance.htm
• Prof. Pogge’s class notes at OSU http://www-astronomy.mps.ohio-state.edu/~pogge/Ast162/Unit4/nebulae.html
• Hubble diagram http://physics.ucsd.edu/students/courses/fall2001/physics5/notes/ch17/sld005.htm
July 27, 2004
Resources
• Inflationary Universe by Alan Guth (Perseus)
• A Short History of the Universe by Joseph Silk (Scientific American Library)
• Before the Beginning by Martin Rees (Perseus)
• Inflation for Beginners (John Gribbin) http://www.biols.susx.ac.uk/Home/John_Gribbin/cosmo.htm
•
July 27, 2004
Remove slides
July 27, 2004
Is the Universe really expanding?
• Take a look at the handout• How do you interpret the 3 graphs?• Try to draw graphs of a Universe that
has– Static galaxies (not moving)– Turbulent galaxies (random motion)– Rotating galaxies (like the planets around
the Sun)– Uniformly contracting galaxies
July 27, 2004
Rules of the game activity
• Analyze the observed particle events to see what the combination rules are