1. 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

3. Enrichment of the Universe with Heavy Elements

4. 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) Nucleosynthesi s Event ? ? ? ? ? ? ? ? ? ? ? background-light sources ionizing source (absorption in) ISM SOFIA VLT XMM-NEWTON INTEGRAL

5. 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 ( 26 Al) Supernova remnant Cassiopeia A

6. Ever increasing precision in observations Cayrel et al. 2004 Log of specific element ratios metallicity Early universe  later universe Co Ni Zn [Zn/Fe] [Ni/Fe] [Co/Fe] [Fe/H] element number abundance log(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

7. 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

8. 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

9. 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

10. 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

11. 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

12. Facility for Antiproton and Ion Research - FAIR GSI today Future 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

13. 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 MPA Observations 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

14. Star formation Ejection of metals Formation of metal-enriched gas clouds How are the ejected elements mixed into the interstellar and intergalactic medium and incorporated into newly formed stars?

15. (Burkert 04, Heitsch et al. 05) KH HI Turbulence and molecular cloud formation

16. 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/USM Turbulence Theory by IPP Observations by MPE, MPA, ESO New Junior Research Group: First light and chemical enrichment of the Universe

17. How did the nuclear composition of galaxies evolve with time? Formation and chemical Evolution of galaxies – matching models and observations –

18. 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

19. 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