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
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