The FAIR* Project *Facility for Antiproton and Ion Research Outline: FAIR layout Research programs Peter Senger, GSI USTC Hefei Nov. 21, 2006 and CCNU.

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