1. Syllabus and slides
Lecture 1: Overview and history of Particle accelerators (EW)
Lecture 2: Beam optics I (transverse) (EW)
Lecture 3: Beam optics II (longitudinal) (EW)
Lecture 4: Liouville's theorem and Emittance (RB)
Lecture 5: Beam Optics and Imperfections (RB)
Lecture 6: Beam Optics in linac (Compression) (RB)
Lecture 7: Synchrotron radiation (RB)
Lecture 8: Beam instabilities (RB)
Lecture 9: Space charge (RB)
Lecture 10: RF (ET)
Lecture 11: Beam diagnostics (ET)
Lecture 12: Accelerator Applications (Particle Physics) (ET)
Visit of Diamond Light Source/ ISIS / (some hospital if possible)
The slides of the lectures are available at
Dr. Riccardo Bartolini (DWB room 622) 1

2. Lecture 10 Synchrotron radiation properties of synchrotron radiation
synchrotron light sources
Lienard-Wiechert potentials
Angular distribution of power radiated by accelerated particles
Angular and frequency distribution of energy radiated:
Radiation from undulators and wigglers
R. Bartolini, John Adams Institute, 8 May 2013

3. What is synchrotron radiation
Electromagnetic radiation is emitted by charged particles when accelerated
The electromagnetic radiation emitted when the charged particles are accelerated radially (v  a) is called synchrotron radiation
It is produced in the synchrotron radiation sources using bending magnets undulators and wigglers
R. Bartolini, John Adams Institute, 8 May 2013

4. Synchrotron radiation sources properties
Broad Spectrum which covers from microwaves to hard X-rays: the user can select the wavelength required for experiment;
synchrotron light
High Flux: high intensity photon beam, allows rapid experiments or use of weakly scattering crystals;
High Brilliance (Spectral Brightness): highly collimated photon beam generated by a small divergence and small size source (partial coherence);
High Stability: submicron source stability
Polarisation: both linear and circular (with IDs)
Pulsed Time Structure: pulsed length down to tens of picoseconds allows the resolution of process on the same time scale
Flux = Photons / ( s  BW)
Brilliance = Photons / ( s  mm2  mrad2  BW )
R. Bartolini, John Adams Institute, 18 May 2011

5. A brief history of storage ring synchrotron radiation sources
First observation:
1947, General Electric, 70 MeV synchrotron
First user experiments:
1956, Cornell, 320 MeV synchrotron
1st generation light sources: machine built for High Energy Physics or other purposes used parasitically for synchrotron radiation
2nd generation light sources: purpose built synchrotron light sources, SRS at Daresbury was the first dedicated machine (1981 – 2008)
3rd generation light sources: optimised for high brilliance with low emittance and Insertion Devices; ESRF, Diamond, …
4th generation light sources: photoinjectors LINAC based Free Electron Laser sources; FLASH (DESY), LCLS (SLAC), …
R. Bartolini, John Adams Institute, 8 May 2013

6. Peak Brilliance diamond
X-rays from Diamond will be 1012 times brighter than from
an X-ray tube,
105 times brighter than the SRS !
X-ray tube
60W bulb
Candle
R. Bartolini, John Adams Institute, 8 May 2013

7. Layout of a synchrotron radiation source (I)
Electrons are generated and accelerated in a linac, further accelerated to the required energy in a booster and injected and stored in the storage ring
The circulating electrons emit an intense beam of synchrotron radiation which is sent down the beamline
R. Bartolini, John Adams Institute, 8 May 2013

8. Layout of a synchrotron radiation source

9. Main components of a storage ring
Insertion devices (undulators) to generate high brilliance radiation
Insertion devices (wiggler) to reach high photon energies
R. Bartolini, John Adams Institute, 8 May 2013

10. Many ways to use x-rays photo-emission (electrons)
electronic structure
& imaging
crystallography
& imaging
diffraction
scattering
SAXS
& imaging
absorption
fluorescence
EXAFS
XRF imaging
Spectroscopy
EXAFS
XANES
& imaging
from the synchrotron
to the detector
Specificity to different elements
R. Bartolini, John Adams Institute, 8 May 2013

11. 3rd generation storage ring light sources
1992 ESRF, France (EU) 6 GeV
ALS, US GeV
1993 TLS, Taiwan 1.5 GeV
1994 ELETTRA, Italy 2.4 GeV
PLS, Korea 2 GeV
MAX II, Sweden 1.5 GeV
1996 APS, US 7 GeV
LNLS, Brazil GeV
1997 Spring-8, Japan 8 GeV
1998 BESSY II, Germany 1.9 GeV
2000 ANKA, Germany 2.5 GeV
SLS, Switzerland 2.4 GeV
2004 SPEAR3, US 3 GeV
CLS, Canada 2.9 GeV
2006: SOLEIL, France 2.8 GeV
DIAMOND, UK 3 GeV
ASP, Australia 3 GeV
MAX III, Sweden 700 MeV
Indus-II, India 2.5 GeV
2008 SSRF, China GeV
2009 PETRA-III, D 6 GeV
2011 ALBA, E 3 GeV
ESRF
SSRF
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12. Diamond Aerial views
June 2003
Oct 2006

13. Heuristic approach to synchrotron radiation
Synchrotron radiation is emitted in an arc of circumference with radius , Angle of emission of radiation is 1/ (relativistic argument), therefore
transit time in the arc of dipole
During this time the electron travels a distance
The time duration of the radiation pulse seen by the observer is the difference between the time of emission of the photons and the time travelled by the electron in the arc
The width of the Fourier transform of the pulse is
R. Bartolini, John Adams Institute, 8 May 2013

14. Lienard-Wiechert Potentials (I)
The equations for vector potential and scalar potential
with the current and charge densities of a single charged particle, i.e.
have as solution the Lienard-Wiechert potentials
[ ]ret means computed at time t’
R. Bartolini, John Adams Institute, 8 May 2013

15. Lineard-Wiechert Potentials (II)
The electric and magnetic fields generated by the moving charge are
computed from the potentials
and are called Lineard-Wiechert fields
velocity field
acceleration field
Power radiated by a particle on a surface is the flux of the Poynting vector
Angular distribution of radiated power [see Jackson]
radiation emitted by the particle
R. Bartolini, John Adams Institute, 8 May 2013

16. velocity  acceleration: synchrotron radiation
Assuming
and substituting the acceleration field [Jackson]
cone aperture
 1/
When the electron velocity approaches the speed of light the emission pattern is sharply collimated forward
R. Bartolini, John Adams Institute, 8 May 2013

17. Total radiated power via synchrotron radiation
Integrating over the whole solid angle we obtain the total instantaneous power radiated by one electron (Larmor formula and its relativistic generalisation)
Strong dependence 1/m4 on the rest mass
proportional to 1/2 ( is the bending radius)
proportional to B2 (B is the magnetic field of the bending dipole)
The radiation power emitted by an electron beam in a storage ring is very high.
The surface of the vacuum chamber hit by synchrotron radiation must be cooled.
R. Bartolini, John Adams Institute, 8 May 2013

18. Energy loss via synchrotron radiation emission in a storage ring
In the time Tb spent in the bendings the particle loses the energy U0
i.e. Energy Loss per turn (per electron)
Power radiated by a beam of average current Ib: this power loss has to be compensated by the RF system
Power radiated by a beam of average current Ib in a dipole of length L
(energy loss per second)
R. Bartolini, John Adams Institute, 8 May 2013

19. The radiation integral (I)
The energy received by an observer (per unit solid angle at the source) is
Using the Fourier Transform we move to the frequency space
Angular and frequency distribution of the energy received by an observer !
Neglecting the velocity fields and assuming the observer in the far field: n constant, R constant
Radiation Integral
R. Bartolini, John Adams Institute, 8 May 2013
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20. The radiation integral (II)
The radiation integral can be simplified to [see Jackson]
How to solve it?
determine the particle motion
compute the cross products and the phase factor
integrate each component and take the vector square modulus
Calculations are generally quite lengthy: even for simple cases as for the radiation emitted by an electron in a bending magnet they require Airy integrals or the modified Bessel functions (available in MATLAB)
R. Bartolini, John Adams Institute, 8 May 2013
20/30 20

21. Radiation integral for synchrotron radiation
Trajectory of the arc of circumference [see Jackson]
In the limit of small angles we compute
Substituting into the radiation integral and introducing
R. Bartolini, John Adams Institute, 8 May 2013
21/30 21

22. Critical frequency and critical angle
Using the properties of the modified Bessel function we observe that the radiation intensity is negligible for  >> 1
Higher frequencies have smaller critical angle
Critical frequency
Critical angle
For frequencies much larger than the critical frequency and angles much larger than the critical angle the synchrotron radiation emission is negligible
R. Bartolini, John Adams Institute, 8 May 2013

23. Frequency distribution of radiated energy
It is possible to verify that the integral over the frequencies agrees with the previous expression for the total power radiated [Hubner]
The frequency integral extended up to the critical frequency contains half of the total energy radiated, the peak occurs approximately at 0.3c
It is also convenient to define the critical photon energy as
For electrons, the critical energy in practical units reads
50%
50%
R. Bartolini, John Adams Institute, 8 May 2013

24. Synchrotron radiation emission as a function of beam the energy
Dependence of the frequency distribution of the energy radiated via synchrotron emission on the electron beam energy
Critical frequency
Critical angle
No dependence on the energy at longer wavelengths
Critical energy ;
for electrons! How does this change for protons?
R. Bartolini, John Adams Institute, 8 May 2013

25. Brilliance with IDs (medium energy light sources)
Brilliance dependence
with current
with energy
with emittance
Medium energy storage rings with in-vacuum undulators operated at low gaps (e.g. 5-7 mm) can reach 10 keV with a brilliance of 1020 ph/s/0.1%BW/mm2/mrad2
25/30
R. Bartolini, John Adams Institute, 8 May 2013

26. Polarisation of synchrotron radiation
Polarisation in the orbit plane
Polarisation orthogonal to the orbit plane
In the orbit plane  = 0, the polarisation is purely horizontal
Integrating on all frequencies we get the angular distribution of the energy radiated
Integrating on all the angles we get a polarization on the plan of the orbit 7 times larger than on the plan perpendicular to the orbit
R. Bartolini, John Adams Institute, 8 May 2013

27. Undulators and wigglers
Periodic array of magnetic poles providing a sinusoidal magnetic field on axis:
Insertion devices (undulators) to generate high brilliance radiation
Constructive interference of radiation emitted by different electrons at different poles
R. Bartolini, John Adams Institute, 8 May 2013
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28. Synchrotron radiation from undulators and wigglers
Continuous spectrum characterized by ec = critical energy
ec(keV) = B(T)E2(GeV)
eg: for B = 1.4T E = 3GeV ec = 8.4 keV
(bending magnet fields are usually lower ~ 1 – 1.5T)
bending magnet - a “sweeping searchlight”
wiggler - incoherent superposition K > 1
Quasi-monochromatic spectrum with peaks at lower energy than a wiggler
undulator - coherent interference K < 1
R. Bartolini, John Adams Institute, 8 May 2013

29. Summary Accelerated charged particles emit electromagnetic radiation
Synchrotron radiation is stronger for light particles and is emitted by bending magnets in a narrow cone within a critical frequency
Undulators and wigglers enhance the synchrotron radiation emission
Synchrotron radiation has unique characteristics and many applications
R. Bartolini, John Adams Institute, 8 May 2013

30. Bibliography
J. D. Jackson, Classical Electrodynamics, John Wiley & sons.
E. Wilson, An Introduction to Particle Accelerators, OUP, (2001)
M. Sands, SLAC-121, (1970)
R. P. Walker, CAS CERN and CAS CERN 98-04
K. Hubner, CAS CERN 90-03
J. Schwinger, Phys. Rev. 75, pg. 1912, (1949)
B. M. Kincaid, Jour. Appl. Phys., 48, pp. 2684, (1977).
R. Bartolini, John Adams Institute, 8 May 2013