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Detection of energetic particles and gamma rays
The interaction of radiation with matter
Peter Dendooven
Basic Detection Techniques 2009-2010http://www.astro.rug.nl/~peletier/DetectionTechniques.html
2
Contents
• Interaction of radiation with matter– high-energy photons
– charged particles• heavy charged particles
• electrons
– neutral particles• neutrons
• neutrinos
• General radiation detection concepts– pulse mode operation
– energy spectrum
– detector efficiency
– timing
• Radiation detectors– semiconductor detectors
• operation principle
• examples (silicon, germanium)
• other materials
– scintillation detectors• principle
• organic scintillators
• inorganic scintillators
• photosensors
– gas detectors• ionisation
• proportional
• Geiger
3
Radiation categories
charged particles
heavy charged particles
fast electrons
neutral particles
high-energy photons
neutrons
neutrinos
“Coulomb”
“easily stopped” transfer
4
Nomenclature high-energy photons
• high-energy photons = energy higher than ionisationenergies, so rougly >1 keV (!<1 nm)
• in principle:
– X-rays: atomic transitions
• up to ~115 keV for uranium
– "-rays: nuclear transitions
• from few eV to many MeV
• other sources of high-energy photons
– bremsstrahlung
– synchrotron radiation
– annihilation radiation
• to keep things simple: “"-rays”
5
High-energy photons: 3 major interactions
• photo-electric effect
• Compton scattering
• pair production
1921
Arthur H. Compton
1927Nobel prizes in physics
6
Attenuation of gamma rays (1/2)
!
I(x) = I0 e"µ x
x
dx
0
I0 I(x)
!
dI
dx" I
!
dI(x)
dx= "µ I(x)
µ: linear attenuation coefficient
all-or-nothing processes:
7
Attenuation of gamma rays (2/2)
mean free path
!
" =x e
-µx dx
0
#
$e
-µx dx
0
#
$=
1
µ
compound or mixture
mass attenuation coefficient
half-thickness
!
µ" #µ
"
!
µ 1
cm
"
# $
%
& ' , (
g
cm3
"
# $
%
& ' ) µ(
cm2
g
"
# $
%
& '
!
µ
"
#
$ % &
' (
c
= wi
i
) µ
"
#
$ %
&
' (
i
wi: weight fraction of element i
!
I(x) = I0 e" ln 2
x
d1/2
!
d1/ 2 =ln2
µcm or
g
cm2
"
# $
%
& '
8
Interaction cross section
number of “interactions” proportional with: N [/s]
– beam intensity I [/s]
– number of “reaction partners” encountered n t (#t’) [/cm2]
beam, I
t
target, n atoms/cm3
N = $ I t’
$= cross section [cm2]
1 barn (b) = 10-24 cm2
9
• interaction with whole atom
• K-electron most probable
• energy deposition:
– (Eb: electron binding energy) % E" > Eb
– electron cloud is “rearranged”:• X-rays
• Auger electrons
– photo-electron preferentially emitted in a forward direction
Photo-electric effect
!
Ee" = E # " E
b
"
!
E "
!
Ee"
10
Photo-electric cross section in lead
absorption edges
11
Compton scattering (1/2)
!
" E # =E #
1+E #
m0c
21$ cos %( )
m0c2 : electron rest mass (511 keV)
& : scattering angle
!
E "
!
" E #
e-
12
Compton scattering (2/2)
angular distribution: Klein-Nishina formula
!
d"
d#($) =
1
2re
2% E &
E &
'
( ) )
*
+ , ,
2
E &
% E &+
% E &
E &
- sin2 $'
( ) )
*
+ , ,
cm2
sr
.
/ 0
1
2 3
!
d"
d#($) =
1
2re
2 1
1+%(1& cos$)
'
( )
*
+ ,
2
1+ cos2 $ +%2(1& cos$)2
1+%(1& cos$)
'
( )
*
+ ,
cm2
sr
-
. /
0
1 2
re: classical electron radius = 2.82 x 10-13 cm
!
" =E #
m0c
2
13
Compton scattering
14
Compton scattering
15
Compton scattering
16
Pair production
• nucleus for momentum conservation
• requires E" > 2 m0c2 = 1022 keV
• kinetic energy (e– + e+) = E" - 1022 keV
• e+ annihilates with an electron
– two 511 keV annihilation photons
– emitted back-to-back
17
Dependence on atomic number and energy
Z : atomic number
photo-electric effect
Compton scattering
pair production
type of interaction attenuation coefficient comment
!
" # Z4.5
E $
-3.5
!
"# Z E $
-1
(0.1 to 10 MeV)
!
" # Z2 E $ %1022 keV( )
!
" # Z2 ln(E $ )
dominates for low energies
and heavy elements
dominates from ~0.5 to 5 MeV
(for most elements)
E close to 1 MeV
E >> 1 MeV
dominates for high
energies and heavy
elements
18
Total "-ray attenuation
µ = ' + $ + (
19
Half-thickness
20
Relative importance
21
Heavy charged particles
• protons, alpha particles, atomic ions
• primary interaction through Coulomb forces
(only at low energy, nuclear reactions are important for energy loss)
• Coulomb scattering by atomic electrons
– maximum energy transfer (head-on collision)
for 10 MeV proton: )Emax * 20 keV
% energy loss in very many small steps
– Coulomb force has infinite range, so interaction with many electrons
simultaneously
% continuous, gradual, energy loss
!
"Emax
# E4m
M
m: electron mass
M: mass heavy particle
22
Heavy charged particles
• Coulomb interaction leads to:
– electron capture/loss by projectile
– exitation projectile
– exitation and ionisation of target atoms
• basis for detection
• kinetic energy is tranferred to +-rays, X-rays, Auger electrons, ...
• many-faceted and complicated process
• paths are essentially straight because
– M >> me
% per interaction a small deflection
– interactions in all directions
23
Stopping power
• stopping power # energy loss per unit of amount of material
• linear stopping power
• specific stopping power
!
S = "dE
dx e.g.
MeV
cm
#
$ %
&
' (
!
S = "dE
d(#x) e.g.
MeV
g cm2
$
% &
'
( )
x
dx
0
E0 E(x)
24
Bethe-Bloch formula
incoming particle: ,: v/c
v: velocity
ze: charge
absorber material: n: electron density (electrons/cm3)
I: average excitation and ionisation potential
~10 Z eV
electron: e: charge
m0: rest mass
!
"dE
dx=
e
4#$0
%
& '
(
) *
2
4# (ze)2 n
m0c2 +2
ln2m0c
2 +2
I" ln 1"+2( ) "+2
,
- .
/
0 1
25
Bethe-Bloch formula
!
"dE
dx= 0.31 MeV cm
2
z2
#2
$ Z
Aln
2m0c
2 #2
I" ln 1"#2( ) "#2
%
& '
(
) *
!
n " N Z "N
A # Z
A
N: atomic density (atoms/cm3)
Z: atomic number
NA: Avogadro constant
-: density (g/cm3)
A: atomic weight
!
"dE
dx=
e
4#$0
%
& '
(
) *
2
4# (ze)2 n
m0c2 +2
ln2m0c
2 +2
I" ln 1"+2( ) "+2
,
- .
/
0 1
26
Stopping power dependencies
non-relativistic Bethe-Bloch
[...] changes slowly
!
"dE
dx#
z2 n
v2
different energy
!
"dE
dx#
1
v2#
1
E
!
"dE
dx# z
2different particle(same velocity)
!
"dE
dx# ndifferent material
!
"dE
dx=
e
4#$0
%
& '
(
) *
2
4# (ze)2 n
m0v2ln
2m0v2
I
+
, -
.
/ 0
27
Bragg-Kleeman rule
stopping power per atom of compounds/mixtures is additive
!
1
Nc
dE
dx
"
# $
%
& '
c
= Wi
1
Nii
( dE
dx
"
# $
%
& '
i
Nc, Ni: atomic density of compound, component
Wi: atomic fraction of component i
28
Stopping power example #1
protons in aluminum
slow-m
oving io
ns
captu
re e
lect
rons
29
Stopping power example #2
about same energy loss minima
% minimum ionizing particle
~2 MeV/(g/cm2) in light materials
30
The Bragg peak
stopping power vs. distance travelled
basis for hadron (e.g. proton) therapy
31
Electrons
electron mass is small
% Coulomb interaction causes:
• large relative energy loss per interaction
• large deviations in path
% large accelerations cause energy loss
due to electromagnetic radiation: bremsstrahlung
% distance travelled >> projected range
% backscattering (low E and high Z)
32
Electron energy loss
!
dE
dx=
dE
dx
"
# $
%
& ' c
+dE
dx
"
# $
%
& ' r
!
"dE
dx
#
$ %
&
' ( c
=e
4)*0
#
$ %
&
' (
2
2) e2 n
m0c2 +2
lnm0v2 E
2I2(1"+2)" (ln2) 2 1"+2 "1++2#
$ %
& ' ( + (1"+2) +
1
81" 1"+2# $ %
& ' (
2,
- .
/
0 1
!
"dE
dx
#
$ %
&
' ( r
=e
4)*0
#
$ %
&
' (
2
e2 n (Z + 1) E
137 m0
2c44 ln
2E
m0c2"
4
3
+
, -
.
/ 0
!
(dE dx)r
(dE dx)c
"E[ MeV] Z
700
c: collisional
r: radiative
33
Electron collisional vs. radiative energy loss
34
Electron stopping power
minimum ionizing particle:
~0.5 to ~5 MeV: 1-2 MeV/(g/cm2)
35
Range of a charged particle
# distance travelled before stopping
!
R = "dE
dx
#
$ %
&
' (
"1
dE
E0
0
)
of more practical use: projected range
(= “range”)
charged particle track
projected range
range
36
Straggling
energy loss is a stochastic process
% energy straggling
% range straggling
% angular straggling
range
37
Range example: hydrogen, helium ions
38
Electron range: examples
39
Cherenkov radiation (1/2)
• a charged particle travelling faster than the speed of light in a
medium emits light, so-called Cherenkov radiation
!
v >c
n
!
" n > 1
!
" #v
c
n: refractive index
• energy threshold
!
Eth
= m0c
2 "1+ 1+1
n2 "1
#
$
% %
&
'
( ( m0c
2: electron rest mass
40
Cherenkov threshold energy
41
Cherenkov radiation (2/2)
• Cherenkov photons are emitted under a fixed angle
!
cos" =1
# n
• yield per unit wavelength . 1/!2
(breaks down at short ! as n%1)
“electromagnetic shock wave”
42
Cherenkov light yield
!
d2N
dE dx" 370 z2 sin2
#(E) 1
eV
1
cmze: charge of particle
43
Cherenkov radiation: example
spent nuclear fuel under water at the La Hague reprocessing plant
44
Neutrons
• no Coulomb interaction, only strong interaction
• short range & atomic nucleus is small:
% interaction probability << than charged particles/photons (~108)
• as the result of an interaction:
– neutron disappears, creating secondary radiation
• mostly heavy charged particles (p,d,t,/) (basis for detection)
– scattering in which energy and direction are significantly changed
• can give rise to recoil nuclei (basis for detection)
% attenuation of a collimated beam is exponential
45
Neutrons
type of interaction depends mostly on the neutron energy
– fast neutrons (> ~0.5 eV)
• elastic scattering (most effective on light nuclei), gives recoil nuclei
• inelastic scattering, gives recoil nuclei
• scattering results in neutron energy loss (neutron is moderated)
• neutron capture (resulting in the emission of charges particles (p,d,t,/))
– resonant
– slow neutrons
• elastic scattering
– small energy loss, so no good for detection, but thermalizes neutrons
(~25 meV at room temperature)
• eventually captured by nucleus followed by gamma ray: (n,")
– most effectively by B, Cd, In, Gd
46
Neutrinos
• no electromagnetic or strong interaction, only weak interaction
% very small interaction probability
e.g. cross section ~ 10-43 cm2
1 cm3 of material contains ~1024 protons
interaction probability ~10-43 x 1024 ~ 10-19 /cm
1019 cm (10 light-years) required for a good capture probability
• neutrino interaction results in secondary radiation,
which is then detected
• interaction possibilities and probabilities are different for the
3 neutrino flavours: electron-, muon-, and tau-neutrino
!
" e + p# n + e+
47
Neutrino detection schemes
• inverse beta-decay– detect e+ (annihilation) and/or Y (radiochemical detection)
• neutrino capture by a nucleus (Homestake experiment)
– detection of 37Ar
• water-Cherenkov detection: scattering off electrons
– all neutrino flavours but with different cross sections
– detected via Cerenkov radiation from the scattered electrons (E0 > 5 MeV)
– Cherenkov cone tells incoming direction and particle type
– e.g. (Super)-Kamiokande
• heavy water: 3 options, all 3 neutrino flavours can be detected
– scattering off electrons (all 3 flavours, different cross sections)
– 0e + d % p + p + e– detect e– via Cherenkov, only 0e
– 0e + d % 0e + n + p deuteron break-up, detect neutron, all 3 flavors,
same cross section
– e.g. SNO (Sudbury Neutrino Observatory)
!
" e+
Z
AX # e
++
Z$1
AY
!
"e+
17
37Cl # e
$+
18
37Ar
!
" + e#$ " + e
#
48
Super-Kamiokande
• 1 000 m underground
• 41.4 m tall, 39.3 m diameter
• 50 000 tonnes ultra-pure water
• 11 146 20” and 1 885 8” photomultiplier tubes
49
Sudbury Neutrino Observatory
• 2 km underground
• 1 000 tonnes of heavy water
• 6-metre radius acrylic vessel
• 9 600 photomultiplier tubes