Download Rare Isotopes ISOTOPES discovery

Rare Isotopes
ISOTOPES discovery
https://www.youtube.com/watch?v=ZvuMRwvJhHw&spfreload=10
How did visible matter come into being and how
does it evolve?
The radioactive galaxy demonstrates the continuing
formation of new radioactive isotopes
A 'snapshot' view of ongoing
nucleosynthesis in the Galaxy by
COMPTEL and INTEGRAL…
26Al
distribution
along galactic
plane
T=7.2·105 yr
Eγ=1.809 MeV
The mean lifetime of 26Al makes the 1.809 MeV gamma-ray line an excellent
tracer for newly synthesized material released into the interstellar medium over
the last several million years
How are atoms cooked in the Cosmos?
Chemical evolution
LOFT (early 2020s ?, ESA)
Hubble
Swift
Chandra
NuSTAR
Most elements are created in violent stellar
explosions, and orbiting and Earth-based
telescopes are capable of measuring these
creation rates.
ce
r-pro
ss
Keck
rp-process
To interpret observations, however, we must
understand reactions occurring in stellar
explosions that create and destroy rare
isotopes.
n-star crust
processes
FRIB, TRIUMF, RIBF, …
Reaction networks
(captures,
Apache
Point decays)
LSST
(High Priority ASTRO 2010)
mass fraction
Chemical evolution
Big
Bang
10
-3
oldest
stars
solar system
r-process
10-6
10-9
10-12
0
50 0
50 100 0
50 100 150 200
0
50 100 150 200
mass number
supernova
neutron star merger
entropy
velocity S. Bruenn et al., ApJ 767, L6 (2012)
http://svs.gsfc.nasa.gov/cgi-bin/details.cgi?aid=10543
S. Rosswog et al., MNRAS 430, 2585 (2013)
Half of the neutron-rich atomic nuclei heavier than iron are
built by neutron driven r-process. The final abundances reflect
the shell structure of nuclei, which determines the respective
nucleosynthesis trajectories.
Curiosity
Mars Rover
– powered
by 238Pu
Quest for understanding the neutron-rich matter on Earth
and in the Cosmos
Crustal structures
Symmetry energy slope
Bounds on EOS
EOS with hyperons
Symmetry energy
Data
The crucial role of High Performance
Computing
Future: large multi-institutional efforts
involving strong coupling between
physics, computer science, and applied
math
Towards predictive capability
W. Nazarewicz
30
hLp://compuZngnuclei.org fusion Validated Nuclear InteracZons Chiral EFT Ab-­‐ini4o Op4miza4on Model valida4on Uncertainty Quan4fica4on Neutron drops Structure and ReacZons: Heavy Nuclei EOS Correla4ons DFT Load balancing Load balancing TDDFT Op4miza4on Eigensolvers Model valida4on Nonlinear solvers Uncertainty Quan4fica4on Model valida4on Eigensolvers Uncertainty Quan4fica4on Nonlinear solvers Mul4resolu4on analysis Structure and ReacZons: Light and Medium Nuclei Stellar burning Neutrinos and Fundamental Symmetries Ab-­‐ini4o RGM CI Neutron Stars Fission 60
Progress in ab-initio calculations
50
40
A
30
20
10
0
1980
1990
2000
Year
2010
2020