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Hans-JÃŒrgen Wollersheim - 2017 Indian Institute of Technology Ropar
Spectral lines of hydrogen
absorption
hydr
ogen
gas
absorption spectrum
Hans-JÃŒrgen Wollersheim - 2017 Indian Institute of Technology Ropar
Element production on the sun
5
Hydrogen emission spectrum
wave length nm
Hans-JÃŒrgen Wollersheim - 2017 Indian Institute of Technology Ropar
Spectral analysis
6
H
Spectral analysis Kirchhoff und Bunsen: Every element has a characteristic emission band
Max Planck
Hans-JÃŒrgen Wollersheim - 2017 Indian Institute of Technology Ropar
Nuclear Resonance Fluorescence
Nuclear Resonance Fluorescence (NRF) is analogous to atomic resonance fluorescence but depends upon the number of protons AND the number of neutrons in the nucleus
Hans-JÃŒrgen Wollersheim - 2017 Indian Institute of Technology Ropar
Photon-nuclear reactions with MeV γ-rays
pure electromagnetic interaction spin selectivity (mainly E1, M1, E2 transitions)
γ-ray
Hans-JÃŒrgen Wollersheim - 2017 Indian Institute of Technology Ropar
Photon-nuclear reactions with MeV γ-rays γ-ray pure electromagnetic interaction
spin selectivity (mainly E1, M1, E2 transitions)
Hans-JÃŒrgen Wollersheim - 2017 Indian Institute of Technology Ropar
Low energy photon scattering at S-DALINAC
âwhiteâ photon spectrum wide energy region examined
Hans-JÃŒrgen Wollersheim - 2017 Indian Institute of Technology Ropar
Principle of measurement and self absorption
Hans-JÃŒrgen Wollersheim - 2017 Indian Institute of Technology Ropar
First γγ-coincidences in a γ-beam
Hans-JÃŒrgen Wollersheim - 2017 Indian Institute of Technology Ropar
First γγ-coincidences in a γ-beam
Hans-JÃŒrgen Wollersheim - 2017 Indian Institute of Technology Ropar
First γγ-coincidences in a γ-beam
Hans-JÃŒrgen Wollersheim - 2017 Indian Institute of Technology Ropar
Total power received by Earth from the Sun
174 Peta (1015) Watt
@ extreme light infrastructure, Europe
Hans-JÃŒrgen Wollersheim - 2017 Indian Institute of Technology Ropar
Compton scattering and inverse Compton scattering
Compton scattering:
Elastic scattering of a high-energy γ-ray on a free electron. A fraction of the γ-ray energy is transferred to the electron. The wave length of the scattered γ-ray is increased: λâ > λ.
âðð ⥠ðððððð2
ðžðžðŸðŸâ² =ðžðžðŸðŸ
1 +ðžðžðŸðŸðððððð2
â 1 â ðððððððð
Inverse Compton scattering:
Scattering of low energy photons on ultra-relativistic electrons. Kinetic energy is transferred from the electron to the photon. The wave length of the scattered γ-ray is decreased: λâ < λ.
ððâ² â ðð â1 â ðœðœ â ðððððððððŸðŸ1 + ðœðœ â ððððððððð¿ð¿
ððâ² â ðð =âðððððð
â 1 â ðððððððððŸðŸ
Hans-JÃŒrgen Wollersheim - 2017 Indian Institute of Technology Ropar
Inverse Compton scattering
Electron is moving at relativistic velocity Transformation from laboratory frame to reference frame of e- (rest frame):
in order to repeat the derivation for Compton scattering
ðžðžðŸðŸ = ðŸðŸ â ðžðžðŸðŸ 1 âð£ð£ððððððððððððâðŸðŸ
Doppler shift
Lorentz factor: ðŸðŸ = 1 â ðœðœ2 â1/2 = 1 + ðððððððððð
931.5â0.00055
ðžðžðŸðŸâ² =ðžðžðŸðŸ
1 +ðžðžðŸðŸðððððð2
â 1 â ðððððððð Compton scattering in rest frame
ðžðžðŸðŸâ² = ðŸðŸ â ðžðžðŸðŸâ² 1 +ð£ð£ððððððððððððâðŸðŸâ²
Limit ðžðžðŸðŸ ⪠ðððððð2
ðžðžðŸðŸâ² â ðŸðŸ2 â ðžðžðŸðŸ 1 âð£ð£ððððððððððððâðŸðŸ 1 +
ð£ð£ððððððððððððâðŸðŸâ²
transformation into the laboratory frame
ðžðžðŸðŸâ² â 4ðŸðŸ2 â ðžðžðŸðŸ
electron and γ interaction ððððâðŸðŸ~1800 γâ emission relative to electron ððððâðŸðŸâ²~00
Hans-JÃŒrgen Wollersheim - 2017 Indian Institute of Technology Ropar
Laser Compton backscattering
Energy â momentum conservation yields ~4ðŸðŸ2 Doppler upshift Thomsons scattering cross section is very small (6·10-25 cm2)
High photon and electron density are required
Hans-JÃŒrgen Wollersheim - 2017 Indian Institute of Technology Ropar
Gamma rays resulting after inverse Compton scattering
A. H. Compton Nobel Prize 1927
photon scattering on relativistic electrons (γ >> 1)
âðð = 2.3 eV â¡ 515 ðððð
ðððððððððð = 720 ðððððð â ðŸðŸðð = 1 +ðððððððððð ðððððð
931.5 â ðŽðŽðð ð¢ð¢= 1410
ðžðžðŸðŸ = 2ðŸðŸðð21 + ððððððððð¿ð¿
1 + ðŸðŸðððððŸðŸ2 + ðð02 + 4ðŸðŸðððžðžð¿ð¿
ðððð2â ðžðžð¿ð¿
4ðŸðŸðððžðžð¿ð¿ðððð2
= recoil parameter
ððð¿ð¿ = ðððžðžððððð¿ð¿ðð
= normalized potential vector of the laser field
E = laser electric field strength ðžðžð¿ð¿ = âððð¿ð¿
ðŸðŸðð = ðžðžðððððð2
= 11âðœðœ2
= Lorentz factor
maximum frequency amplification: head-on collision (ΞL = 00) & backscattering (Ξγ = 00)
ðžðžðŸðŸ~4ðŸðŸðð2 â ðžðžð¿ð¿ â 18.3 ðððððð
Hans-JÃŒrgen Wollersheim - 2017 Indian Institute of Technology Ropar
Scattered photons in collision
Luminosity: ð¿ð¿ = ððð¿ð¿âðððð4ððâððð ð
2
ððð¿ð¿ = 0.5 ðœðœ âððð¿ð¿ = 2.4 ðððð = 3.86 â 10â19 ðœðœ â¡ 515 ðððð
â ððð¿ð¿= 1.3 â 1018
ððð ð = 15 ðððð
ðð = 1 ðððð
â ðððð= 6.25 â 109
â ðð
γ-ray rate: ðððŸðŸ = ð¿ð¿ â ððððððððððððððð ðððð = 0.67 â 10â24 ðððð2
â 2.9 â 1032 â ðð ððððâ2ððâ1
â 2 â 108 â ðð ððâ1 (full spectrum)
Yb: Yag J-class laser
10 Peta (1015) Watt
repetition rate: ðð = 3.2 ðððððð
Hans-JÃŒrgen Wollersheim - 2017 Indian Institute of Technology Ropar
Thomson Scattering
J. J. Thomson Nobel prize 1906
Thomson scattering = elastic scattering of electromagnetic radiation by an electron at rest â the electric and magnetic components of the incident wave act on the electron â the electron acceleration is mainly due to the electric field â the electron will move in the direction of the oscillating electric field â the moving electron will radiate electromagnetic dipole radiation â the radiation is emitted mostly in a direction perpendicular to the motion of the electron â the radiation will be polarized in a direction along the electron motion
Hans-JÃŒrgen Wollersheim - 2017 Indian Institute of Technology Ropar
Thomson Scattering
J. J. Thomson Nobel prize 1906
ðððððð ððððΩ
=12ðð02 â 1 + ðððððð2ðð
ðð0 =ðð2
4ðððð0ðððððð2= 2.818 â 10â15 ðð
ðððð = ï¿œðððððð ððððΩ
ððΩ =2ðððð02
2ï¿œ 1 + ðððððð2ðð ðððððð
0
=8ðð3ðð02 = 6.65 â 10â29 ðð2 = 0.665 ðð
differential cross section
classical electron radius
Hans-JÃŒrgen Wollersheim - 2017 Indian Institute of Technology Ropar
Scattered photons in collision
Ξ = 0 Ξ = Ï
ðžðžðŸðŸ = 2ðŸðŸðð21 + ððððððððð¿ð¿
1 + ðŸðŸðððððŸðŸ2 + ðð02 + 4ðŸðŸðððžðžð¿ð¿
ðððð2â ðžðžð¿ð¿
ððð ð ðððð = 1/ðŸðŸ
Hans-JÃŒrgen Wollersheim - 2017 Indian Institute of Technology Ropar
Inverse Compton scattering of laser light
Hans-JÃŒrgen Wollersheim - 2017 Indian Institute of Technology Ropar
Extreme Light Infrastructure â Nuclear Physics
Hans-JÃŒrgen Wollersheim - 2017 Indian Institute of Technology Ropar
Nuclear Resonance Fluorescence
Widths of particle-bound states: Π†10ðððð
Breit-Wigner absorption resonance curve for isolated resonance:
ðððð ðžðž = ððï¿œÌ ï¿œð22ðœðœ + 1
2Î0Î
ðžðž â ðžðžðð 2 + Î 2â 2 ~ Î0 Îâ
Resonance cross section can be very large: ðð0 â 200 ðð (for Î0 = Î, 5 MeV)
Example: 10 mg, A~200 â Ntarget = 3·1019, Nγ = 100, event rate = 0.6 [s-1]
Hans-JÃŒrgen Wollersheim - 2017 Indian Institute of Technology Ropar
Nuclear Resonance Fluorescence
Count rate estimate 104 γ/(s eV) in 100 macro pulses 100 γ/(s eV) per macro pulse example: 10 mg, A ~ 200 target resonance width Π= 1 eV 2 excitations per macro pulse 0.6 photons per macro pulse in detector pp-count rate 6 Hz 1000 counts per 3 min
8 HPGe detectors 2 rings at 900 and 1270
εrel(HPGe) = 100% solid angle ~ 1% photopeak εpp ~ 3%
narrow band width 0.5%
Hans-JÃŒrgen Wollersheim - 2017 Indian Institute of Technology Ropar
Nuclear Resonance Fluorescence
narrow bandwidth allows selective excitation and detection of decay channels
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