Christian Stegmann, Cosmology, CERN 2008 Time Cosmology Cosmology Christian Stegmann University of...

Christian Stegmann, Cosmology, CERN 2008

CosmologyCosmology Christian StegmannUniversity of Erlangen-Nuremberg

Big Bang today

The Earth …The Earth …Heute

… … one of eight planetsone of eight planetstoday

StarsStarstoday

The Milky Way ...The Milky Way ...today

... full of stars... full of starstoday

and nebulaeand nebulaetoday

Our Milky WayOur Milky Waytoday

The Universe is full of galaxiesThe Universe is full of galaxiestoday

Galaxy clusterGalaxy clustertoday

Edwin Hubbles DiscoveryEdwin Hubbles Discovery

• Galaxies travel away from us

• the further away, the faster

Galaxies are moving Galaxies are moving today

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!

Timetoday

some time later

How do we measure this?How do we measure this?

• Measurement of the velocity– velocity-meter?

• Distance– Ruler?

Measurement of the velocity via the Measurement of the velocity via the red-shiftred-shift

Cosmological red shiftCosmological red shift

Space is expanding

Galaxy-spektroscopyGalaxy-spektroscopy

Calcium

Magnesium

Sodium

Galaxy-spektrum

Star-spektrum

vGalaxy ~ 12000 km/s

Distance measurementDistance measurement

apparent brightness ~ true brightness . 1/R2

distance, R

brightness

known distance

measuredbrightness

One point andall is determined

measuredbrightness

measureddistance

We need lamps!We need lamps!

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

Where is the supernova?Where is the supernova?today

Here!Here!today

„„Standard candles“Standard candles“today

The Hubble-DiagramThe Hubble-Diagram

red shift (velocity)

• The Universe is expanding (acclerating)!• The Universe was smaller at earlier times

• The Universe was created in a hot phase

The Big Bang

World modelsWorld models

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

Space curvatureSpace curvaturetoday

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

Distribution of galaxiesDistribution of galaxiestoday

The accelerated UniverseThe accelerated Universe

• Einsteins cosmological constant

• cosmological constant acts like an anti-gravitation

A travel through the timeA travel through the time

First there was …First there was …0

From Big Bang until todayFrom Big Bang until today0

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

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

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

NukleosynthesisNukleosynthesis

• Age = 1 min, T = 109 K– Generation of light

elements– Hydrogen, Deuterium,

Helium, Lithium

Nuclear fusionNuclear fusion

• Fusion in collisions

• Fusion requries high temperatures and large densities

particle distanceForv

Strong electo-static repulsion at intermediate distances

Strong nuclear attraction at smal distances

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

Generation of atomsGeneration of atoms

• Age = 370000 Jahre, T = 3000 Kelvin– First atoms generated– The Universe becomes transparent

370000 years

Can we see the Big Bang?Can we see the Big Bang?

370000 years

Back into the pastBack into the past

4 light years

370000 years

2 million light years

370000 years

some billions of light years

Each view into the Universe isa view back into the past

Back into the pastBack into the past

370000 Jahre

The Big Bang fills the skyThe Big Bang fills the sky

The Big Bang past - nowThe Big Bang past - now

Past:Light 3000 K

today:Mikrowaves 3 K

370000 years

1965 – The discovery1965 – The discovery

Microwave radiation from the cosmos

370000 years

COBE and WMAPCOBE and WMAP

• COBE– COsmic Background Explorer

– 1989 – 1993

– Nobel price 2006 (G. Smoot, J. Mather)

• WMAP– Wilkinson Microwave Anisotropy

– Start 2001

370000 years

The microwave backgroundThe microwave background

T = 2.7 K

370000 years

T = 0,0035 K

The Earth is movingThe Earth is moving370000 years

The spectrumThe spectrum370000 years

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

T = 0,000018 K

The echo of the big bangThe echo of the big bang370000 years

Multipol expansionMultipol expansion370000 years

The power spectrumThe power spectrum370000 years

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

Matter

Neutrinos

Neue Formvon Energie

Neue Formvon Materie

370000 Jahre

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!

Doppler effectDoppler effect

low frequency

red shift

high frequency

blue shift

Spektra for identificationSpektra for identificationtoday

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

Geometry of the UniverseGeometry of the Universe

• Balance between contraction and expansion expresse by Ω0 = ρ/ρkrit

– Ω0 > 1, ρ > ρkritGravitation wins, Universe collapse

– Ω0 = 1, ρ = ρkritExpansion eventually stopps

– Ω0 < 1, ρ < ρkritExpansion wins, Universum is expanding forever

• Λ > 0, fate of the Universe not connected to the geometry

Why not in stars?Why not in stars?

Fusion in starsFusion in stars1 min

• Erwarte ungefähr genauso viel Helium wie andere Elemente mit großer Masse– Verhältnis: 75% H, 13% He, 12% Rest

Fusion in starsFusion in stars

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

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

Kosmologische ParameterKosmologische Parameter370000 Jahre

Dunkle MaterieDunkle Materie

• Rotationskurven von Galaxien

• Elliptische Galaxien

• Gravitationslinsen

• Mikrowellen-Hintergrund

RotationskurvenRotationskurvenHeute

Galaxien-Cluster 1E 0657-Galaxien-Cluster 1E 0657-5656

optisch

Galaxien-Cluster 1E 0657-Galaxien-Cluster 1E 0657-5656

Röntgen

GravitationslinsenGravitationslinsen

Optisch + Röntgen + Dunkle Materie

Was ist passiert?Was ist passiert?

Galaxien Cluster CL0024 17Galaxien Cluster CL0024 17Heute

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