Cosmology Christian Stegmann University of Erlangen-Nuremberg
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Transcript of Cosmology Christian Stegmann University of Erlangen-Nuremberg
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Christian Stegmann, Cosmology, CERN 2008
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CosmologyCosmology Christian StegmannUniversity of Erlangen-Nuremberg
Big Bang today
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Christian Stegmann, Cosmology, CERN 2008
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The Earth …The Earth …Heute
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Christian Stegmann, Cosmology, CERN 2008
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… … one of eight planetsone of eight planetstoday
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Christian Stegmann, Cosmology, CERN 2008
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StarsStarstoday
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Christian Stegmann, Cosmology, CERN 2008
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The Milky Way ...The Milky Way ...today
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Christian Stegmann, Cosmology, CERN 2008
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... full of stars... full of starstoday
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Christian Stegmann, Cosmology, CERN 2008
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and nebulaeand nebulaetoday
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Christian Stegmann, Cosmology, CERN 2008
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Our Milky WayOur Milky Waytoday
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Christian Stegmann, Cosmology, CERN 2008
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The Universe is full of galaxiesThe Universe is full of galaxiestoday
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Christian Stegmann, Cosmology, CERN 2008
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Galaxy clusterGalaxy clustertoday
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Christian Stegmann, Cosmology, CERN 2008
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Edwin Hubbles DiscoveryEdwin Hubbles Discovery
• Galaxies travel away from us
• the further away, the faster
today
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Christian Stegmann, Cosmology, CERN 2008
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Galaxies are moving Galaxies are moving today
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Christian Stegmann, Cosmology, CERN 2008
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Do we understand that?Do we understand that?
• We are the centre of the Universe!
• The Universe is expanding– Space between galaxies is getting larger
Scientifically more attractive!
today
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Christian Stegmann, Cosmology, CERN 2008
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today
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Christian Stegmann, Cosmology, CERN 2008
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some time later
today
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Christian Stegmann, Cosmology, CERN 2008
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How do we measure this?How do we measure this?
• Measurement of the velocity– velocity-meter?
• Distance
– Ruler?
today
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Christian Stegmann, Cosmology, CERN 2008
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Measurement of the velocity via the Measurement of the velocity via the red-shiftred-shift
today
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Christian Stegmann, Cosmology, CERN 2008
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Cosmological red shiftCosmological red shift
Space is expanding
today
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Christian Stegmann, Cosmology, CERN 2008
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Galaxy-spektroscopyGalaxy-spektroscopy
Calcium
Magnesium
Sodium
Galaxy-spektrum
Star-spektrum
vGalaxy ~ 12000 km/s
today
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Christian Stegmann, Cosmology, CERN 2008
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Distance measurementDistance measurement
apparent brightness ~ true brightness . 1/R2
R
today
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Christian Stegmann, Cosmology, CERN 2008
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distance, R
brightness
known distance
measuredbrightness
One point andall is determined
measuredbrightness
measureddistance
today
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Christian Stegmann, Cosmology, CERN 2008
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We need lamps!We need lamps!
today
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Christian Stegmann, Cosmology, CERN 2008
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Star explosionsStar explosions
• Supernova Typ Ia• Exploding white dwarfs
– nuclear bomb of the size of the Earth!
• Bright as a whole galaxy
• Light up and disappear after a few weeks
Supernova 1994D
today
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Christian Stegmann, Cosmology, CERN 2008
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Where is the supernova?Where is the supernova?today
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Christian Stegmann, Cosmology, CERN 2008
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Here!Here!today
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Christian Stegmann, Cosmology, CERN 2008
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„„Standard candles“Standard candles“today
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Christian Stegmann, Cosmology, CERN 2008
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The Hubble-DiagramThe Hubble-Diagram
red shift (velocity)
Dis
tan
ce
Heute
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Christian Stegmann, Cosmology, CERN 2008
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• The Universe is expanding (acclerating)!
• The Universe was smaller at earlier times
• The Universe was created in a hot phase
The Big Bang
today
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Christian Stegmann, Cosmology, CERN 2008
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World modelsWorld models
today
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Christian Stegmann, Cosmology, CERN 2008
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General relativityGeneral relativity
• Einstein 1916• Describes all gravitationally bound
systems– planets– black holes – the Universe
• Mass produces curvature of the space• Curvature tells masses how to move
→ gravitation
today
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Christian Stegmann, Cosmology, CERN 2008
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Space curvatureSpace curvaturetoday
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Christian Stegmann, Cosmology, CERN 2008
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SolutionSolution
• Cosmological principle– We see what every other sees – Isotrop and homogeneous
Universe
• Friedmann Universe (1922)
• World models depend only on – Expansion – Gravitational attraction
Homogeneous but not isotrop
Isotrop but not homogeneous
Isotrop AND homogeneous
Heute
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Christian Stegmann, Cosmology, CERN 2008
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Distribution of galaxiesDistribution of galaxiestoday
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Christian Stegmann, Cosmology, CERN 2008
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The accelerated UniverseThe accelerated Universe
• Einsteins cosmological constant
• cosmological constant acts like an anti-
gravitation
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Christian Stegmann, Cosmology, CERN 2008
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A travel through the timeA travel through the time
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Christian Stegmann, Cosmology, CERN 2008
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First there was …First there was …0
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Christian Stegmann, Cosmology, CERN 2008
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From Big Bang until todayFrom Big Bang until today0
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Christian Stegmann, Cosmology, CERN 2008
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A time travelA time travel
• Age = 10-42 s– The beginning of physics
• Age = 10-36 s, T = 1027 K– Strong and electroweak force decouple
10-42 s
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Christian Stegmann, Cosmology, CERN 2008
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The inflationThe inflation
• Age = 10-36 s, T = 1021 K – Sudden expansion of the Universe by a factor 1020 – 1030
– The Universe gets flat!
10-36s
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Christian Stegmann, Cosmology, CERN 2008
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The battleThe battle
• Age = 10-6 s, T = 1012 Kelvin– Matter and antimatter annihilate
– Matter-antimatter-ratio
100000001 : 10000000
– Matter-photon-ratio
1 : 100000000
10-6 s
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Christian Stegmann, Cosmology, CERN 2008
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NukleosynthesisNukleosynthesis
• Age = 1 min, T = 109 K– Generation of light
elements
– Hydrogen, Deuterium, Helium, Lithium
1 min
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Christian Stegmann, Cosmology, CERN 2008
Time
Nuclear fusionNuclear fusion
• Fusion in collisions
• Fusion requries high temperatures and large densities
particle distanceFo
rvc
e
Strong electo-static repulsion at intermediate distances
Strong nuclear attraction at smal distances
1 min
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Christian Stegmann, Cosmology, CERN 2008
Time
Primordiale NukleosynthesisPrimordiale Nukleosynthesis
• Explains the abundances of light elements
– 74% Hydrogen
– 25% Helium
– 1% other
• Baryonic density
– 3,5∙10-31 g/cm3 or
– 0,2 Hydrogen atoms/m3
1 min
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Christian Stegmann, Cosmology, CERN 2008
Time
Generation of atomsGeneration of atoms
• Age = 370000 Jahre, T = 3000 Kelvin– First atoms generated
– The Universe becomes transparent
370000 years
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Christian Stegmann, Cosmology, CERN 2008
Time
Can we see the Big Bang?Can we see the Big Bang?
370000 years
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Christian Stegmann, Cosmology, CERN 2008
Time
Back into the pastBack into the past
4 light years
370000 years
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Christian Stegmann, Cosmology, CERN 2008
Time
2 million light years
370000 years
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Christian Stegmann, Cosmology, CERN 2008
Time
some billions of light years
Each view into the Universe isa view back into the past
Back into the pastBack into the past
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Christian Stegmann, Cosmology, CERN 2008
Time
370000 Jahre
The Big Bang fills the skyThe Big Bang fills the sky
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Christian Stegmann, Cosmology, CERN 2008
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The Big Bang past - nowThe Big Bang past - now
Past:Light 3000 K
today:Mikrowaves 3 K
370000 years
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Christian Stegmann, Cosmology, CERN 2008
Time
1965 – The discovery1965 – The discovery
Microwave radiation from the cosmos
370000 years
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Christian Stegmann, Cosmology, CERN 2008
Time
COBE and WMAPCOBE and WMAP
• COBE
– COsmic Background Explorer
– 1989 – 1993
– Nobel price 2006 (G. Smoot, J.
Mather)
• WMAP
– Wilkinson Microwave Anisotropy
Probe
– Start 2001
370000 years
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Christian Stegmann, Cosmology, CERN 2008
Time
The microwave backgroundThe microwave background
T = 2.7 K
370000 years
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Christian Stegmann, Cosmology, CERN 2008
Time
T = 0,0035 K
The Earth is movingThe Earth is moving370000 years
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Christian Stegmann, Cosmology, CERN 2008
Time
The spectrumThe spectrum370000 years
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Christian Stegmann, Cosmology, CERN 2008
Time
The history of the cosmic The history of the cosmic background radiationbackground radiation
observer
Surface of last scattering
Edge of the visible Universe.black body radiation
The visible Universe
black body radiation
370000 years
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Christian Stegmann, Cosmology, CERN 2008
Time
T = 0,000018 K
The echo of the big bangThe echo of the big bang370000 years
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Christian Stegmann, Cosmology, CERN 2008
Time
Multipol expansionMultipol expansion370000 years
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Christian Stegmann, Cosmology, CERN 2008
Time
The power spectrumThe power spectrum370000 years
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Christian Stegmann, Cosmology, CERN 2008
Time
Cosmological ParameterCosmological Parameter
– Total energiy density 1.003 ± 0.015
– Matter density 0.24 ± 0.04
– Baryon density 0.042 ± 0.004
– Vakuum energy density 0.76 ± 0.05
– Neutrino density < 0.014
– Age of the Universe 13.7 ± 0.2 Gyr
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Christian Stegmann, Cosmology, CERN 2008
Time
60%
40%
20%
0%
80%
100%
Matter
Neutrinos
Stars
Neue Formvon Energie
Neue Formvon Materie
370000 Jahre
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Christian Stegmann, Cosmology, CERN 2008
Time
SummarySummary
• Our Universe was created in a Big Bang
– Galaxy move away from us
– Abundances of light elements
– Cosmic microwave background
• 97% of the energy density of the Universe is
unknown!
today
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Christian Stegmann, Cosmology, CERN 2008
Time
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Christian Stegmann, Cosmology, CERN 2008
Time
Doppler effectDoppler effect
low frequency
red shift
high frequency
blue shift
today
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Christian Stegmann, Cosmology, CERN 2008
Time
Spektra for identificationSpektra for identificationtoday
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Christian Stegmann, Cosmology, CERN 2008
Time
Parameter of an expanding UniverseParameter of an expanding Universe
• Expansion ↔ Gravitational acceleration
• Expansion– Hubble constant H0 is a measure for the strength of the
expansion: H0 = 20 km/s/MLj
• Gravitational acceleration– Normal matter slows down the expansion (mean density
ρ)
– critical density, requried to stop expansion:
ρkrit = 3 H02/8πG = 10-29 g/cm3
today
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Christian Stegmann, Cosmology, CERN 2008
Time
Geometry of the UniverseGeometry of the Universe
• Balance between contraction and expansion expresse by Ω0 = ρ/ρkrit
– Ω0 > 1, ρ > ρkrit
Gravitation wins, Universe collapse– Ω0 = 1, ρ = ρkrit
Expansion eventually stopps– Ω0 < 1, ρ < ρkrit
Expansion wins, Universum is expanding forever
• Λ > 0, fate of the Universe not connected to the geometry
today
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Christian Stegmann, Cosmology, CERN 2008
Time
Why not in stars?Why not in stars?
1 min
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Christian Stegmann, Cosmology, CERN 2008
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Fusion in starsFusion in stars1 min
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Christian Stegmann, Cosmology, CERN 2008
Time
•
• Erwarte ungefähr genauso viel Helium wie andere Elemente mit großer Masse– Verhältnis: 75% H, 13% He, 12% Rest
Fusion in starsFusion in stars
Zeit
Ker
n T
em
pe
ratu
r
107 K
108 K
109 K
Wasserstoff-Brennen
Helium-Brennen
carbon-burning
1.5x107 K
6x108 K
1x108 K
H Brenn-SchaleHe Brenn-Schale
C Brenn-SchaleO Brenn-SchaleSi Brenn-Schale
Fe Kern- keine Fusion
1 min
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Christian Stegmann, Cosmology, CERN 2008
Time
Vergleich Stellarer und Vergleich Stellarer und Primordialer NukleosynthesePrimordialer Nukleosynthese
109 : 11:1Photon-Baryon-Verhältnis
10-5 g/cm3
(wie die Luft in diesem Raum)
100 g/cm3Dichte
FallendAnsteigendTemperatur-entwicklung
MinutenMilliarden von Jahren
Zeitskala
Primordiale Nukleosynthese
Stellare Nukleosynthese
1 min
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Christian Stegmann, Cosmology, CERN 2008
Time
Kosmologische ParameterKosmologische Parameter370000 Jahre
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Christian Stegmann, Cosmology, CERN 2008
Time
Dunkle MaterieDunkle Materie
• Rotationskurven von Galaxien
• Elliptische Galaxien
• Gravitationslinsen
• Mikrowellen-Hintergrund
Heute
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Christian Stegmann, Cosmology, CERN 2008
Time
RotationskurvenRotationskurvenHeute
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Christian Stegmann, Cosmology, CERN 2008
Time
Galaxien-Cluster 1E 0657-Galaxien-Cluster 1E 0657-5656
optisch
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Christian Stegmann, Cosmology, CERN 2008
Time
Galaxien-Cluster 1E 0657-Galaxien-Cluster 1E 0657-5656
Röntgen
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Christian Stegmann, Cosmology, CERN 2008
Time
GravitationslinsenGravitationslinsen
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Christian Stegmann, Cosmology, CERN 2008
Time
Optisch + Röntgen + Dunkle Materie
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Christian Stegmann, Cosmology, CERN 2008
Time
Was ist passiert?Was ist passiert?
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Christian Stegmann, Cosmology, CERN 2008
Time
Galaxien Cluster CL0024 17Galaxien Cluster CL0024 17Heute