The FAIR* Project *Facility for Antiproton and Ion Research Outline: FAIR layout Research programs...
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Transcript of The FAIR* Project *Facility for Antiproton and Ion Research Outline: FAIR layout Research programs...
The FAIR* Project*Facility for Antiproton and Ion Research
Outline: FAIR layout Research programs
Peter Senger, GSI
USTC Hefei Nov. 21, 2006 and CCNU Wuhan, Nov. 23, 2006
storage and cooler rings
• beams of rare isotopes• e – A Collider
• 1011 stored and cooled antiprotons
0.8 - 14.5 GeV
primary beams
• 5x1011/s; 1.5-2 GeV/u; 238U28+
• factor 100-1000 increased intensity• 4x1013/s 90 GeV protons• 1010/s 238U 35 GeV/u ( Ni 45 GeV/u)
secondary beams
• rare isotopes 1.5 - 2 GeV/u; factor 10 000 increased intensity • antiprotons 3(0) - 30 GeV
The Facility for Antiproton and Ion Research
accelerator technical challenges
•Rapidly cycling superconducting magnets•high energy electron cooling•dynamical vacuum, beam losses
accelerator physics high intensive heavy ion beams dynamical vacuum rapidly cycling superconducting magnets high energy electron cooling
Research programmes at FAIR
Rare isotope beams; nuclear structure and nuclear astrophysics nuclear structure far off stability nucleosynthesis in stars and supernovae
Beams of antiprotons: hadron physics quark-confinement potential search for gluonic matter and hybrids hypernuclei
high-energy nucleus-nucleus collisions: compressed baryonic matter
baryonic matter at highest densities (neutron stars) phase transitions and critical endpoint in-medium properties of hadrons pulsed heavy ion beams: plasma physics matter at high pressure, densities, and temperature fundamentals of nuclear fusion
atomic physics and applied research highly charged atoms low energy antiprotons radiobiology
M 8M
red giant white dwarf
Onion shell structure before explosion
Birth and dead of stars
8M M 15M
Supernova II1.4M Mcore 2M
neutron star
M 15M
Supernova IIaM 2M
black hole
The origin of elements
number of neutrons
nu
mb
er
of
pro
ton
s
Nucleosynthesis in core-collapse supernova-explosions:
rapid neutron capture by unstable (neutron-rich ) isotopes
Fusion in stars
NuSTAR: Nuclear Structure, Astrophysics, Reactions
Intensive rare isotope beams produced by in-flight projectile fragmentation/fission
Hadron physics with high energy antiprotons
Search for gluonic excitations:
Search for in-medium modifications of hadron properties
Precision γ-spectroscopy of single and double hypernuclei
Study of the confinement potential with charmonium spectroscopy:
1 fm C C
Charmonium spectroscopy
3500 3520 MeV3510
CB
all
ev./
2 M
eV
100
ECM
CBallE835
1000
E 8
35
ev./
pb
c1
e+e- versus pp
The PANDA Detector
charging cyclotron
cooling section
electron gunand collector
accelerationcolumn
return beamline
High-energy-electron-cooling
energy 0.4 - 8 MeVcurrent up to 2 A
magnetic field 0.2 - 0.5 T(Supercond. Solenoids)in cooling section 30 m
Electrostatic Accelerator, charged by H– beam from cyclotron
Inertia l fusion (fue l)Inertia l
fusion (converte r)
M agnetic fusion
p lasm a
S olar corona
Tem
pe
ratu
re [
eV]
Density [cm ]-3
P H ELIXnhelix
S un (cente r)
so lid sta tedensity
H eavy-ionheated gas
targe ts(R FQ )
S un (surface)
Jupite r (cente r)
B row n dw arf
G SI gas-d ischarge p lasm as
B eamH eating(S IS-18)
B eamH eating(S IS-200)
The phase diagram of atomic matter
The phase diagram of strongly interacting matter