The FAIR Chance for Nuclear Astrophysics Elemental Abundances Core-collapse Supernovae The neutrino process The r-process nuclei in -Wind Neutron Stars in Binaries

100 m UNILAC SIS 18 SIS 100/300 HESR Super FRS NESR CR RESR GSI today Future facility ESR FLAIR Rare-Isotope Production Target Antiproton Production Target CBM PP / AP CN DE ES FI FR GB GR IN IT PL RO RU SE Observers

100 m UNILAC SIS 18 SIS 100/300 HESR Super FRS NESR CR RESR GSI today New facility FAIR ESR FLAIR Rare-Isotope Production Target Antiproton Production Target CBM PP / AP Ion beams today: Z = 1 – 92 (Protons til uranium) Up to 2 GeV/nucleon Ion beams today: Z = 1 – 92 (Protons til uranium) Up to 2 GeV/nucleon Future beams: Intensity: primary ions 100-fold secondary RIB fold Types : Z = -1 – 92 (Antiprotons til uranium) Energies: ions up to GeV/u antiprotons GeV/c Future beams: Intensity: primary ions 100-fold secondary RIB fold Types : Z = -1 – 92 (Antiprotons til uranium) Energies: ions up to GeV/u antiprotons GeV/c

FAIR Start Event: November 7, 2007 A splendid perspective and eminent challenge !

Mass measurements at FAIR

We are made of star stuff Carl Sagan Each heavy atom in our body was build and processed through ~ star generations since the initial Big Bang event!

Signatures of Nucleosynthesis nucleosynthesis processes nucleosynthesis history of our universe solar abundance distribution The stellar abundance distribution is a reflection of nuclear structure and nuclear stability!

Solar Elemental Abundances

The Cosmic Cycle

Evolution of a Star

Stellar Life

Simulation of Supernova Collapse Electron capture on nuclei Composition: increasingly neutron rich nuclei Elastic neutrino scattering on nuclei Courtesy: RIKEN

Weak interaction during collapse phase

Effects of Nuclear Electron Capture during Core Collapse The electron capture at high densities results in lower Y e and generates neutrino wind which is necessary for driving the shock. Hix, Messer, Mezzacappa, et al ‘03 Electron captures on nuclei dominate

Two-Dimensional Supernova Simulation Plasma instabilities Equation of State Neutrino transport –Neutrino opacities –Dense matter correlations –Neutrino-nucleon reactions Rotation, magnetic fields..... courtesycourtesy Courtesy Hans-Thomas Janka Courtesy: Hans-Thomas Janka

Needs for Supernova Simulations Plasma Instabilities Equation of State Electron Capture on Nuclei Neutrino-nucleus Reactions

Explosive Nucleosynthesis Neutrino-Proton Process (early ejecta, proton rich) R-Process (late ejecta, neutron rich) Neutrino reactions with nucleons determine the proton-to-neutron ratio

Possible consequences of high neutrino flux in shock-front Neutrino capture on protons 1 H( +,e + )n, neutron production which influence the reaction path by neutron capture. Anti-neutrino capture on protons produce neutrons at late times (n,p) reactions simulate beta decays and overcome waiting points

p-process in hydrogen rich, high neutron flux environments On-site neutron production through neutrino induced interaction: 1 H( +,e + )n! By-passing waiting point nuclei 64 Ge, 68 Se by n-capture reactions.

The R-Process Masses Half lives Neutron capture rates Fission Neutrino reactions Courtesy: K.-L. Kratz

Supernova shock front nucleosynthesis

R-Process Simulation Courtesy: Gabriel Martinez-Pinedo

FAIR Chance: Nuclear masses R-Process abundances depend on neutron separation energies Different mass models predict different patterns FRDM: ‚robust‘ patterns, as observed in old halo stars in Milky Way ETFSI: individual patterns strongly depending on neutron-to-seed ratios

Mass measurements at FAIR

FAIR Chance: Role of Halflives Competition velocity of ejected matter vs. halflives IF halflives were known, strong constraint of matter ejection from neutron star surface!

FAIR Chance: Neutron Stars Neutron Stars are laboratories for matter at extreme densities Neutron rich nuclei Equation of State for nuclear matter Exotic phases?

X-Ray Burst and RP-Process

Fate of ashes on neutron star surface Neutron star surface ashes ocean Inner crust outer crust H,He gas cooling Radiative cooling Nuclear reactions thermonuclear Electron capture thermonuclear pycnonuclear

Increase with Z 1  Z 2 superbursts 34 Ne 1.5 x g/cm 3 68 Ca 1.8 x g/cm Ge 56 Ar 2.5 x g/cm x g/cm 3 72 Ca 4.4 x g/cm 3 rp-ashes 106 Pd 56 Fe Ouellette, Gupta & Brown 2005 Haensel & Zdunik 1990, 2003 Beard & Wiescher 2003 Known mass Crust processes

The FAIR Chance: New Horizons