Transcript Lecture1(SynchrotronRadiationI) - Indico

Electron beam dynamics in storage rings
Synchrotron radiation
and its effect on electron dynamics
Lecture 1: Synchrotron radiation
Lecture 2: Undulators and Wigglers
Lecture 3: Electron dynamics-I
Lecture 4: Electron dynamics-II
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Contents
Introduction
properties of synchrotron radiation
synchrotron light sources
Lienard-Wiechert potentials
Angular distribution of power radiated by accelerated particles
non-relativistic motion: Larmor’s formula
relativistic motion
velocity  acceleration: synchrotron radiation
Angular and frequency distribution of energy radiated:
the radiation integral
radiation integral for bending magnet radiation
Radiation from undulators and wigglers
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
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;
Flux = Photons / ( s  BW)
High Brilliance (Spectral Brightness): highly collimated photon beam
generated by a small divergence and small size source (partial coherence);
Brilliance = Photons / ( s  mm2  mrad2  BW )
High Stability: submicron source stability
Polarisation: both linear and circular (with IDs)
Pulsed Time Structure: pulsed length down to tens of picoseconds allows the
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resolution
of process on the same time scale
diamond
1.E+20
1.E+18
1.E+16
2
2
Brightness (Photons/sec/mm /mrad /0.1%)
Peak Brilliance
1.E+14
1.E+12
X-rays from Diamond
will be 1012 times
brighter than from
an X-ray tube,
105 times brighter
than the SRS !
1.E+10
1.E+08
1.E+06
X-ray
tube
60W bulb
Candle
1.E+04
1.E+02
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
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Layout of a synchrotron radiation source (II)
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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), …
• 5th generation light sources: FELS driven by LPWA…very speculative
3rd generation storage ring light sources
1992
ESRF, France (EU)
6 GeV
ALS, US
1.5-1.9 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
1.35 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, Australia3 GeV
MAX III, Sweden
700 MeV
Indus-II, India
2.5 GeV
2008
SSRF, China
3.4 GeV
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2011
ALBA, Spain
3 GeV
ESRF
SSRF
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Diamond Aerial views
June 2003
Oct 2006
Main components of a storage ring
Dipole magnets to bend the electrons
Sextupole magnets to focus off-energy
electrons (mainly)
Quadrupole magnets to focus the electrons
RF cavities to replace energy losses due to
the emission of synchrotron radiation
Main components of a storage ring
Insertion devices (undulators) to
generate high brilliance radiation
R. Bartolini, John Adams Institute, 12 November 2014
Insertion devices (wiggler) to
reach high photon energies
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Many ways to
use x-rays
photo-emission
(electrons)
electronic structure
& imaging
diffraction
crystallography
& imaging
scattering
SAXS
& imaging
absorption
from the synchrotron
to the detector
Spectroscopy
EXAFS
XANES
& imaging
fluorescence EXAFS
XRF imaging
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Applications
Medicine, Biology, Chemistry, Material Science, Environmental Science and more
Biology
Reconstruction of the 3D structure of a nucleosome
with a resolution of 0.2 nm
The collection of precise information on the molecular
structure of chromosomes and their components can
improve the knowledge of how the genetic code of
DNA is maintained and reproduced
R. Bartolini, John Adams Institute, 12 November 2014
Archeology
A synchrotron X-ray beam at the SSRL facility
illuminated an obscured work erased, written over
and even painted over of the ancient
mathematical genius Archimedes, born 287 B.C.
in Sicily.
X-ray fluorescence imaging revealed the
hidden text by revealing the iron contained in
the ink used by a 10th century scribe. This xray image shows the lower left corner of the
page.
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Lienard-Wiechert Potentials (I)
The equations for vector potential and scalar potential
1  2

 2


c t 2
0
2
1 2 A
J
 A 2 2  2
c t
c 0
2
with the current and charge densities of a single charged particle, i.e.
 ( x , t )  e (3) ( x  r (t ))
J ( x , t )  ev (t ) (3) ( x  r (t ))
have as solution the Lienard-Wiechert potentials
 ( x ,t ) 

1 
e
40  ( 1    n )R  ret
[ ]ret means computed at time t’
t  t '
R (t ' )
c
A( x ,t ) 


e
40 c  ( 1    n )R  ret
1
Lineard-Wiechert Potentials (II)
The electric and magnetic fields generated by the moving charge are
computed from the potentials
A
E  V 
B   A
t
and are called Lineard-Wiechert fields

e 
n 
e  n  (n   )   
E (x, t) 



40   2 (1    n ) 3 R 2  ret 40 c  (1    n ) 3 R 
ret
velocity field
acceleration field
B ( x ,t ) 
1

R
1

nE
c


E  B  nˆ
Power radiated by a particle on a surface is the flux of the Poynting vector
S
1
0
E B
  ( S )(t )   S ( x , t )  n d

Angular distribution of radiated power [see Jackson]
d 2P
 ( S  n)(1  n   ) R 2
d
radiation emitted by the particle
rit
Angular distribution of radiated power:
non relativistic motion
Assuming
  0 and substituting the acceleration field
 n  (n   ) 
Eacc ( x , t ) 


40 c 
R
 ret
e
2
d 2P
1
e2
)

REacc 
n

(
n


d  0 c
4 2  0 c
2
2
d 2P
e2

2


sin

d (4 ) 2  0c
 is the angle between the acceleration and the observation direction
Integrating over the angles gives the total radiated power
P
e2
60 c

2
Larmor’s formula
Angular distribution of radiated power:
relativistic motion
Substituting the acceleration field
2
d 2P
1
e2

REacc 
d o c
4 2  0 c

n  (n   )  
(1  n   )5

2
emission is peaked in the
direction of the velocity
The pattern depends on the details of velocity and acceleration but it is
dominated by the denominator
Total radiated power: computed either by integration over the angles or by
relativistic transformation of the 4-acceleration in Larmor’s formula
P
e2
60 c

 6 (  ) 2  (    ) 2

Relativistic generalization of
Larmor’s formula
velocity  acceleration: synchrotron radiation
Assuming
  
d 2P
e2

d 4 2  0c 2
and substituting the acceleration field

n  (n   )  
(1  n   )5

2
e 
2
2
1

4 2  0c (1   cos  )3

sin 2  cos 2  
1  2
2
  (1   cos  ) 
cone aperture
 1/
When the electron velocity approaches the speed of light the emission
pattern is sharply collimated forward
velocity  acceleration: synchrotron radiation
Courtesy K. Wille
Total radiated power via synchrotron radiation
Integrating over the whole solid angle we obtain the total instantaneous
power radiated by one electron
2
e2  2 E
e2
dp 2 e 2c  4
e4

4
2 2
P
  





E
B
4
2 3
2
4 5
60c
60c
Eo
60 m c dt
60 
60 m c
e2
4
2
• 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.
Energy loss via synchrotron radiation emission
in a storage ring
In the time Tb spent in the bendings
the particle loses the energy U0
2 e 2  4
U 0   Pdt  PTb  P

c
3 0 
i.e. Energy Loss per turn (per electron)
e 2 4
E (GeV ) 4
U 0 (keV ) 
 88.46
3 0 
 (m)
Power radiated by a beam of average
current Ib: this power loss has to be
compensated by the RF system
I b  Trev
e
4
e
E (GeV ) 4 I ( A)
P(kW ) 
I b  88.46
3 0 
 (m)
N tot 
Power radiated by a beam of average
e 4
L(m) I ( A) E (GeV ) 4
P(kW ) 
LI b  14.08
current Ib in a dipole of length L
60  2
 (m) 2
(energy loss per second)
The radiation integral (I)
The energy received by an observer (per unit solid angle at the source) is


d 2W
d 2P
 
dt  c 0  | RE (t ) |2 dt
d  d

Using the Fourier Transform we move to the frequency space

d 2W
 2c 0  | RE ( ) |2 d
d
0
Angular and frequency distribution of the energy received by an observer
2
d 3W
2 ˆ
 2 0cR E ( )
dd
Neglecting the velocity fields and assuming the observer in the far field:
n constant, R constant
2


3
2
dW
e
n  ( n   )   i ( t  n  r ( t ) / c )
Radiation Integral

e
dt
2
2

dd 40 4 c  (1  n   )


The radiation integral (II)
The radiation integral can be simplified to [see Jackson]
d 3W
e 2 2

dd 40 4 2 c

2
i ( t  n  r ( t ) / c )
n

(
n


)
e
dt


How to solve it?
 determine the particle motion
r (t );  (t );  (t )
 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)
Radiation integral for synchrotron radiation
Trajectory of the arc of circumference [see Jackson]
 

c 
c
r (t )    1  cos t , sin
t , 0 
 

 

In the limit of small angles we compute


 ct 
 ct 
    cos
 sin  
n  (n   )     || sin 
  
  


   ct 

 n  r (t ) 
 cos  
 t 
   t  sin 
c 

 c   

Substituting into the radiation integral and introducing
2


2 2 3/ 2

1


 
3
3c

d 3W
e 2  2 
 2 2
2 2 2
2
2



1



K
(

)

K
(

)
1/ 3
 2/3

2 2
d d 16 3 0 c  3c 2 
1







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Critical frequency and critical angle
2

d 3W
e 2  2 
 2 2
2 2 2
2
2



1



K
(

)

K
(

)
1/ 3
 2/3

2 2
d d 16 3 0 c  3c 2 
1







Using the properties of the modified Bessel function we observe that the
radiation intensity is negligible for  >> 1


2 2 3/ 2

1


   1
3c 3
Higher frequencies
have smaller critical
angle
3c 3

2
Critical frequency
c 
Critical angle
1  
c   c 

1/ 3
For frequencies much larger than the critical frequency and angles much
larger than the critical angle the synchrotron radiation emission is negligible
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Frequency distribution of radiated energy
Integrating on all angles we get the frequency distribution of the energy
radiated
dW
d 3I
3e 2 

d 

d 
d

d

4

c
C
0
4
dW
e 2   



d 40c  c 

K

 
/
5/ 3
( x)dx
C
1/ 3
 << c
1/ 2
    / c
dW
3 e

   e
d
2 40 c  c 
2
 >> c
often expressed in terms of the
function S() with  = /c

9 3
S ( ) 
  K 5 / 3 ( x)dx
8 
dW
3e 2 

d 40c c

 S ( )d  1
0

2 e 2
K 5 / 3 ( x)dx 
S ( )

9 0c
 / c
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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]



U 0 1 dW
1 2e 2
e 2c  4
P
 
d 
c   d  K 5 / 3 ( x)dx 
Tb Tb 0 d
Tb 9 0c 0
6 0c  2

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
 c  c 
3 c 3

2 
For electrons, the critical energy in practical
units reads
50% 50%
E [GeV ]3
 c [keV ]  2.218
 0.665  E[GeV ]2  B [T ]
[m]
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Polarisation of synchrotron radiation
2

d 3W
e 2  2 
 2 2
2 2 2
2
2



1



K
(

)

K
(

)
1/ 3
 2/3

2 2
d d 16 3 0 c  3c 2 
1







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

d 2W
d 3I
7e 2 5
1

d 
d 0 d d
640  (1   2 2 )5 / 2
 5  2 2 
1 
2 2
 7 1   
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
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Synchrotron radiation from undulators and wigglers
(more in lecture 16)
Continuous spectrum characterized
by c = critical energy
bending magnet - a “sweeping searchlight”
c(keV) = 0.665 B(T)E2(GeV)
eg: for B = 1.4T E = 3GeV c = 8.4 keV
(bending magnet fields are usually
lower ~ 1 – 1.5T)
wiggler - incoherent superposition K > 1
Quasi-monochromatic spectrum with
peaks at lower energy than a wiggler
undulator - coherent interference K < 1
u  K 2  u
n 
1
 2
2 
2n 
2  n
nE[GeV ]2
 n (eV )  9.496
 K2 
u [m] 1 

2


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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
3c 3
c 

2
Critical angle
No dependence on
the energy at longer
wavelengths
1  
c   c 

1/ 3
Critical energy
 c  c 
3 c 3

2 
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
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
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 94-01 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).