Nucleosynthesis Predictions and High-Precision Deuterium ...
Klhi L kKarlheinz Langanke GSI Helmholtzzentrum Darmstadt ...the production of energy in stars and...
Transcript of Klhi L kKarlheinz Langanke GSI Helmholtzzentrum Darmstadt ...the production of energy in stars and...
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How Nature makes goldThe role of isotopes for the origin of the elements
K lh i L kKarlheinz LangankeGSI Helmholtzzentrum Darmstadt
AAAS Symposium, Vancouver, February 20, 2012
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Signatures of NucleosynthesisSignatures of Nucleosynthesissolar abundance distributionsolar abundance distribution
NUCLEAR ASTROPHYSICS is concerned with
the origin of elements in stellar burning
the production of energy in stars and stellar explosio
• nucleosynthesis processes • nucleosynthesis history
of our universe
the production of energy in stars and stellar explosio
1010
stellar H-, He, C, O, Si-burning
stars, supernovae
s-processHe-burning in AGB stars, of our universe
100
105
Abun
danc
e
cosmic rays
p-process
r-process
type II supernovae,merging neutron stars
He-burning in AGB stars, massive stars
observational signatures are
abundance distributions
0 50 100 150 200A
10-5
p-processsite disputedThe stellar abundance
distribution is a reflection of nuclear structure and n clear stabilit ! abundance distributions
luminosities
nuclear stability!
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What is an Isotope?What is an Isotope?
F i b fFor a given number ofprotons, isotopes differby their number of neutronsunstable due to beta decay
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Nucleosynthesis processesNucleosynthesis processes
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Star at the end of its lifeStar at the end of its life
Star has an onion like structureStar has an onion-like structure
Iron is the end-product of stellar burning
After nuclear energy sourceAfter nuclear energy sourcehas ceased, stellar corecollapses under its gravity
SUPERNOVA
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Supernova collapse and explosionSupernova collapse and explosion
In about a second, the core radius ,reduces from 6000 km to 20 km
Collpase stops when the inner coreCollpase stops when the inner corecorresponds to a gigantic nucleuswith about half of a solar mass.
fMost of the gain in gravitationalenergy is released in the explosion.This energy corresponds to thegy pproduction of 100 Suns during theirentire life of 10 Billion years.
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Supernova SimulationSupernova Simulation
• Recent progress:p g• Multi-dimensional
hydrodynamicshydrodynamics• Improved nuclear
inputp– Electron capture– Neutrino-induced
reactions
cCourtesy Hans-Thomas Janka
Courtesy: Hans-Thomas Janka
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Electron capture during collapseElectron capture during collapse
Capture rates on nucleivs free protons
Modern many-body models predict electron capture rates whichdiffer by more than a magnitude from previous estimates.
Consequence: capture on (unstable) neutron-rich isotopes dominatethrough the entire collapse with significant impact on neutrino spectrathrough the entire collapse with significant impact on neutrino spectraand temperature-density profiles of the core
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Stellar electron captureStellar electron capture
Stable nuclei are unstable under stellar conditions
Data from charge-exchange reactions: (n,p), (d,2He)
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Making radioactive isotopesMaking radioactive isotopes
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(p,n) charge-exchange reactions on rare isotopesM. Sasano, R.G.T. Zegers et al. PRL 107, 202501 (2011)
Extract Gamow-Teller strengths model-independently• Weak reaction rates for late stellar evolution (supernovae)
First successful experiment: 56Ni(p,n)to extract Gamow-Teller strengths for supernova unstable isotope
New method for (p,n) in inverse kinematics: applicable t ti l i f d it ti
n
RI beam
to exotic nuclei of any mass and excitation energy.•Inverse kinematics•Requires beam intensities >104 pps•Explore very neutron rich nuclei in next generation RI beam f ili i lik FRIB@MSUfacilities like FRIB@MSU
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Neutron Stars: supernova remnantsNeutron Stars: supernova remnants
• Neutron Stars areNeutron Stars are laboratories for matter at extreme densities
• Neutron rich nuclei• Equation of State for
nuclear matter• Exotic phases?
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Explosive hydrogen burningExplosive hydrogen burningBinary system of compact object andBinary system of compact object andcompanion star in hydrostatic burning.Mass flow induces thermonuclear explosion
White Dwarf – NovaNeutron Star – x-ray burster
Observation of gamma lines; e.g. fromelectron-positron annihilation followingbeta+ (positron) decay of unstable nuclei like 18F
Integral satellite
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Novae: Explosive H burningp g
TUDA
18F(p,)15ODRAGON
Affects 22Na and 26gAl radioisotope ejecta from classical novae
reduced uncertainty for 511 keVspectrum in classical novae
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Precision mass measurementsPrecision mass measurements
Isoltrap at CERN
Penning trap
Mass measurements performed inJyvaeskylae, Finland, for rp-process
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Rp-process massesRp process masses
R flRp-process mass flow
Effect on abundance predictions
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Making Gold!Making Gold!
Nature
vsvs
Humans
Old stars in galactic halo have the samer-process abundances as the solar system
Johann Friedrich Böttger, AlchemistInventor of European White Chinar process abundances as the solar system
for A>130, but not below.
two distinct r-process sites?
Inventor of European White ChinaIn Meissen, Germany
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The R-ProcessThe R Process
• Masses• Half lives• Neutron capture ratesNeutron capture rates• Fission• Neutrino reactionsNeutrino reactions
Courtesy: K -L KratzCourtesy: K.-L. Kratz
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Potential r-process sitesPotential r process sites
Neutrino-driven wind from a Neutron star mergersNeutrino-driven wind from anascent neutron star in a supernova explosion
Neutron star mergers
Freiburghaus et al.
Woosley et al.
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R-Process at high entropy: fissionR Process at high entropy: fission
Courtesy: Gabriel Martinez-Pinedo
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Next-Generation Isotope FacilitiesNext Generation Isotope Facilities
TRIUMF/ISAC
MSU/FRIBGSI/FAIR
RIKEN/RIBF
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UNILACSIS 18
SIS 100/300GSI today New facility FAIR
SuperFRS
ESR Rare-IsotopeProduction Target
CBM
HESR
FRS
AntiprotonProduction TargetPP / AP
CRRESR
FLAIR
AP
Future beams:Intensity: primary ions 100-fold
d RIB 10000 f ld
Future beams:Intensity: primary ions 100-fold
d RIB 10000 f ld
100 m
NESR
CR
Ion beams today:Z = 1 – 92(Protons til uranium)
Ion beams today:Z = 1 – 92(Protons til uranium)
secondary RIB 10000-fold Types : Z = -1 – 92(Antiprotons til uranium) Energies: ions up to 35 45 GeV/u
secondary RIB 10000-fold Types : Z = -1 – 92(Antiprotons til uranium) Energies: ions up to 35 45 GeV/u100 m(Protons til uranium)
Up to 2 GeV/nucleon(Protons til uranium)Up to 2 GeV/nucleon
Energies: ions up to 35 - 45 GeV/uantiprotons 0 -15 GeV/c
Energies: ions up to 35 - 45 GeV/uantiprotons 0 -15 GeV/c
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Mass measurements at FAIRMass measurements at FAIR
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The RIB Chance: New HorizonsThe RIB Chance: New Horizons