Cluster of Excellence: Origin and Structure of the Universe

Research Area G:

How was the Universe enriched in heavy elements?

R. Krücken

TU München & MLL

A. Burkert, H. Böhringer, R. Diehl, D. Habs, G. Hasinger, W. Hillebrandt, H.-Th. Janka, R. Krücken, G. Kauffmann, M. Kissler-Patig, B. Leibundgut , E. Müller, W.C. Müller, F. Primas, G. Raffelt, P. Ring, M. Teshima, P. Thirolf, S.D.M. White, H. Wolter

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Research Area A

Big Bang

The History of the UniverseThe History of the UniverseThe History of the UniverseThe History of the Universe

10

-43

s

Todaytime

© Cluster of Excellence - Origin and Structure of the Universe

13

bil

lion

years

10

-34

s

10

-10

s

300 s

30

0.0

00

years

1 b

illi

on

years

Superstring /Supergravity Era

GUT EraCosmic Inflation?

Electro-weak &Quark Era

Particles Era

Radiation dominated Era Matter dominated Era

Research Area B

Research Area C

Research Area D

Research Area G

Research Area F

Research Area E

Star & GalaxyFormation

Present

Decoupling ofMatter - Radiation

np

QQ

Q

Q

Zϒ

e-

ϒ

n p

np BlackHoles

ϒ

First light from Big Bang emergesFirst Supernovae

& heavy elements

Protons and neutrons formNucleosynthesis of He

Electromagnetcic& weak forces decouple

Particles responsible for strong, weak and electro-magnetic forces emerge

Forces and energy are

indistinguishable (speculative)

Universe grows from atomic to cosmic scale in

thousands of a second

Enrichment of the Universe with Heavy Elements

Measuring Cosmic Abundances

Meteoritic-Grain / Ocean crust Mass Spectrometry

Molecular Absorption-lines (Radio,IR)

Atomic Absorption-lines (opt,UV)

Atomic Emission-lines(opt,UV,X)

Nuclear Lines (Radioactive-Isotope Gamma-Rays)

Nucleosynthesis Event

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background-lightsources

ionizing source

(absorption in)

ISM

SOFIA

VLT

XMM-NEWTON

INTEGRAL

Elemental or Isotopic distributions on large and small scales

Chandra (Hwang et al. 2004)

X-ray Images in atomic Lines

Gas-phase oxygen abundance in ~53400 galaxies vs. mass

Complete CGRO Mission (Plüschke et al. 2001)

Gamma-ray Images in Isotopic Lines (26Al)

Supernova remnant Cassiopeia A

Ever increasing precision in observations

Cayrel et al. 2004

Log

of s

peci

fic e

lem

ent

ratio

s

metallicity

Early universe later universe

Co

Ni

Zn

[Zn

/Fe]

[Ni/

Fe]

[Co

/Fe]

[Fe/H]

40 50 60 70 80 90-2

-1

0

1

element number

abun

danc

e lo

g(X

/H)-

12

CS22892-052 (Sneden et al. 2003)

solar r

Other finding:• Metal-poor stars have same r-process pattern as sun

despite many matter cycles for the sun

Indication for robust r-process mechanism independent to specific event

Main Questions in Research Area G

• How do stars explode?

• How are the heavy elements formed in such explosions?

• How are the ejected elements mixed into the interstellar and intergalactic medium and incorporated into newly formed stars?

• How did the nuclear composition of galaxies evolve with time?

Observations Modeling

Laboratory Experiments

How do stars explode?

Crab Nebula

Next steps: Modeling nucleosynthetic output of the explosions improve models for more massive stars towards 3D models

Example: Neutrino-driven Explosion of ONeMg Cores

How do stars explode?

GOAL:

Development of improved explosion models that are tested against more precise observations and can be

used for diagnosis of individual events.

Models by MPA

Observations by ESO, MPE

Theory on EoS by LMU

How are the heavy elements formed in such explosions?

In early phase:• Proton-rich neutrino-driven wind (p-process)

Later:• Neutrino-driven neutron-rich outflow (r-process)

Nucleosynthesis in SN explosions

Explosive nucleosynthesis runs through exotic nuclei

Nuclear shell structure- Defines r-process path- Imprinted in abundance pattern

- Fission may fill the holes- Depends on shell structure as well

Facilities for radioactive ion beams: Access to properties of r-process nuclei Towards a unified description of nuclei(today: CERN/ISOLDE, GSI Darmstadt, ILL Grenoble;Future: FAIR (Darmstadt), RIBF (Japan)

r - process

Facility for Antiproton and Ion Research - FAIR

GSI todayGSI today

Future FacilityFuture Facility

Secondary Beams

• Broad range of radioactive beams

up to 1.5 - 2 GeV/u; • up to factor 10 000 in intensity over present

• Antiprotons 3 - 30 GeV

Reach of mass measurements

How are the heavy elements formed in such explosions?

GOALS:Development of improved model predictions of

nucleosynthesis cross-checked against observations of large scale surveys and of individual events

Models by MPAObservations by MPE, ESO

Improved understanding of shell structure of very exotic nuclei involved in explosive nucleosynthesis

Laboratory experiments by MLL (LMU, TUM)Nuclear theory by MLL (LMU, TUM) GSI

New W2 Professorship for experimental Nuclear Astrophysics

Starformation

Ejection of metalsFormation of

metal-enrichedgas clouds

How are the ejected elements mixed into the interstellar and intergalactic medium and incorporated into newly formed stars?

(Burkert 04, Heitsch et al. 05)

KH

HI

Turbulence and molecular cloud formation

How are the ejected elements mixed into the interstellar and intergalactic medium and incorporated into newly

formed stars?

GOAL:

Development of improved models of molecular cloud and star formation

Simulations by LMU/USMTurbulence Theory by IPP

Observations by MPE, MPA, ESO

New Junior Research Group: First light and chemical enrichment of the Universe

How did the nuclear composition of galaxies evolve with time?

Formation and chemical Evolution of galaxies – matching models and observations –

How did the nuclear composition of galaxies evolve with time?

GOALS:

High precision observational data on element specific abundances through large surveys

Analysis of observational data by ESO, MPA, MPE

Improved models of galactic evolution and their chemical enrichment

Large scale simulations of chemical evolution of galaxies by MPA

Summary

Goal for the next 5 years:

Better understanding of

the enrichment of the universe with heavy elements

by

interlinking and enhancing the existing expertise in

modeling, observations, and laboratory experiments