Simulations of Particle Interactions with Matter

Class Admin

Forest_SimPart_Syllabus

The ability to simulate nature using a computer has become a useful skill for physicists who work in disciplines ranging from basic research to video games. This class will teach you these fundamentals using a practical approach, based on a specific UNIX based programming environment, to simulate fundamental physics processes ranging from ionization and the photoelectric effect to producing anti-matter.

Homework

Homework is due at the beginning of class on the assigned day. If you have a documented excuse for your absence, then you will have 24 hours to hand in the homework after released by your doctor.

Class Policies

http://wiki.iac.isu.edu/index.php/Forest_Class_Policies

Instructional Objectives

Course Catalog Description

Simulations of Particle Interactions with Matter 3 credits. Lecture course with monte-carlo computation requirements. Topics include: Stopping power, interactions of electrons and photons with matter, hadronic interactions, and radiation detection devices.

Prequisites:Math 3360. Phys 3301 or 5561.

Course Description

A practical course applying theoretical descriptions of fundamental particle interactions such as the photoelectric effect, compton scattering and pair production to describe multiple interactions of particles with matter using the montecarlo method. A software package known as GEANT from CERN will be used that is freely available under the UNIX environment. The course assumes that the student has very limited experience with the UNIX environment and no experience with GEANT. Homework problems involve modifying and compiling example programs written in C++. A final project is required in which the student chooses a process to compare the predictions of GEANT with experimental data. A report is written in a format that would be publishable in a scientific journal. Publishing the report is not required but left as an option for the student.

Objectives and Outcomes

SPIM_ObjectiveNoutcomes

Homework Problems

HomeWork_Simulations_of_Particle_Interactions_with_Matter

Introduction

TF_SPIM_Intro

Energy Loss

TF_SPIM_StoppingPower

Ann. Phys. vol. 5, 325, (1930)

Interactions of Electrons and Photons with Matter

Bremsstrahlung

Definition

Radiation produced when a charged particle is deflected by the electric field of nuclei in a material.

Note: There is also electron-electron brehmstrahlung but the interaction is with the electric field of the materials atomic electrons.

The Cross section formula is given in Formula 3Cs, pg 928 of reference H.W. Koch & J.W Motz, Rev. Mod. Phys., vol 31 (1959) pg 920 as

Note

Bethe & Heitler first calculated this radiation in 1934 which is why you will sometimes hear Bremsstrahlung radiation refererd to as Bethe-Heitler.

[math]d \sigma = 4 Z^2r_e^2 \alpha \frac{d \nu}{\nu} \left \{ \left (1 + \left( \frac{E}{E_0} \right )^2 \right ) \left [ \frac{\phi_1(\gamma)}{4} - \frac{1}{3} \ln Z -f(Z)\right ] - \frac{2E}{3E_0} \left [ \frac{\phi_2(\gamma)}{4} - \frac{1}{3} \ln Z -f(Z)\right ] \right \} [/math]

where

[math]E_0[/math] = initial total energy of the electron

[math]E[/math] = final total energy of the electron

[math]\nu = \frac{E_0-E}{h}[/math] = energy of the emitted photon

[math]Z[/math] = Atomic number = number of protons in target material

[math]\gamma = \frac{100 m_ec^2 h \nu}{E_0 E Z^{1/3}}[/math] = charge screening parameter

Coulomb correction to using the Born approximation (approximation assumes the incident particle is a plane wave interacting with a static E-field the correction accounts for changes iin the plane wave due to the presence of the field) Charge screening and the coulomb correction are different effects that have been shown to be additive/independent. File:Haug 2008.pdf

[math]f(Z) = (Z \alpha)^2 \sum_1^{\infty} \frac{1}{ n [ n^2 + (Z \alpha)^2]}[/math]

[math]\sim (Z \alpha)^2 \left \{ \frac{1}{1+(Z \alpha)^2} +0.20206 - 0.0369(Z \alpha)^2 + 0.0083 (Z \alpha)^4 - 0.002 (Z \alpha)^6\right \}[/math]

[math]\alpha = \frac{1}{137}[/math]

[math]\phi_1[/math] and [math]\phi_2[/math] = screening functions that depend on Z

if [math]Z \ge 5[/math]

[math]\phi_1(\gamma) = 20.863 - 2 \ln[1+(0.55 \gamma)^2] - 4[1-0.6e^{-0.98} - 0.4e^{-3 \gamma/2}][/math]

[math]\phi_2(\gamma) = \phi_1(\gamma) - \frac{2}{3}(1+6.5 \gamma + 6 \gamma^2)[/math]

For Z<5 see Tsai, Rev.Mod. Phys., vol 46 (1974) pg 815

if [math]3 \ge Z \lt 5[/math] use Equation 3.46 and 3.47

if [math] Z \lt 2[/math] use Equation 3.25 and 3.26

Note

Energy loss via Bethe-Bloch is due to coulomb deflection and is a continuous process while Bremsstrahlung is a discrete process (emission of photons)

We now know 2 ways charged particles can loose energy when passsing through matter.

Energy loss

[math]\left ( \frac{dE}{dx} \right )_{tot} = \left ( \frac{dE}{dx} \right )_{rad} + \left ( \frac{dE}{dx} \right )_{col}[/math]

[math]{rad} \Rightarrow[/math] : Bremsstrahlung

[math]{col} \Rightarrow[/math] : Bethe-Bloch (collision)

[math]-\left ( \frac{dE}{dx} \right )_{rad} = N \int_o^{\nu_0} \left ( h \nu \right ) \left ( \frac{d \sigma}{d \nu} \right ) d \nu[/math]

where

[math]N = \frac{ number\; atoms}{cm^3} = \frac{\rho N_a}{A} = \frac{density \;\times\; Avagadros\;\;Number}{Atomic number}[/math]

[math]\left ( h \nu \right )[/math] = Energy of emmitted photon

[math]\left ( \frac{d \sigma}{d \nu} \right )[/math] = Probabitlity of Energy loss

The quantity[math] \Phi_{rad} [/math] is defined such that

[math]\Phi_{rad} \equiv \frac{1}{E_0} \int_o^{\nu_0} \left ( h \nu \right ) \left ( \frac{d \sigma (E_0,\nu)}{d \nu} \right ) d \nu[/math]

[math]\Phi_{rad}[/math] is a macroscopic function of a given material rather than just the energy [math]\nu[/math] which we will use to define a common property of materials known as the radiation length [math]\left ( R_0=\frac{1}{N\Phi_{rad}} \right )[/math]

[math]\Phi_{rad} = 4Z^2r_e^2 \alpha \left \{ { \left [ \ln(\frac{2E}{m_ec^2}) - \frac{1}{3} - f(z) \right ] \gamma \gt \gt 1 \atop \left [ \ln(183E^{-1/3}) + \frac{1}{18} - f(z) \right ] \gamma \sim 0} \right .[/math]

where

[math]\gamma \gt \gt 1[/math] case is no screening and [math]1 \ll \frac{E_0}{m_e c^2} \lt \frac{1}{\alpha Z^{1/3}}[/math]

[math]\gamma \; \sim \; 0[/math] case has [math] \frac{E_0}{m_e c^2} \gg \frac{1}{\alpha Z^{1/3}}[/math]

The energy loss equation becomes

[math]- \frac{dE}{dx} = N E_0 \Phi_{rad}[/math]

Note

for intermediate value of [math]\gamma[/math] you need to integrate numerically

[math]\left ( \frac{dE}{dx} \right )_{rad}\propto Z^2E[/math] : Bremsstrahlung

[math]\left ( \frac{dE}{dx} \right )_{col}\propto Z \ln (E)[/math] : Bethe-Bloch

The illustration below shows the relative contributions of Bethe-Bloch and Bremsstrahlung to the total energy loss according to the above functional dependence. At low energies the physics of collisions dominates the loss (Bethe-Bloch) and as energy increases the discrete loss by radiation begins to dominate.

Critical Energy[math] E_C[/math]

At the critical energy [math]E_C[/math] the two energy loss processes contribute equally to the total energy lost by a charged particle interacting with matter.

[math]E_C \equiv[/math] energy at which [math]\left ( \frac{dE}{dx} \right )_{rad} = \left ( \frac{dE}{dx} \right )_{col}[/math]

In the PDG

[math]E_C \sim \frac{800 MeV}{Z+1.2}[/math]

Examples

Critical Energy E_C
Material	[math]E_C[/math] (MeV)
Pb	9.51
Fe	27.4
Cu	24.8
Al	51

Electron-Electron Bremsstrahlung

Electron electron bremsstrahlung

The radiation produced as 2 electrons pass near eachother

[math]d \sigma[/math] is essentially the same except you have [math]z=1[/math] thereby adding a [math]Z[/math] term and not a [math]Z^2[/math] term

reference:pg 947 from Koch and Motz, Rev. Mod. Phys, vol 31 (1959) pg 920 File:SPIM Koch andMotz RevModPhysv31 1959pg920.pdf

as a result

[math]d \sigma_{tot} = \frac{Z(Z+1)}{Z^2} d \sigma_{Brem}[/math]

= [math]4 Z(Z+1)r_e^2 \alpha \frac{d \nu}{\nu} \left \{ \left (1 + \left( \frac{E}{E_0} \right )^2 \right ) \left [ \frac{\phi_1(\gamma)}{4} - \frac{1}{3} \ln Z -f(Z)\right ] - \frac{2E}{3E_0} \left [ \frac{\phi_2(\gamma)}{4} - \frac{1}{3} \ln Z -f(Z)\right ] \right \} [/math]

Most calculations ignore electron-electron Brehmsstrahung because its linear in Z and doesn;t become important until low Z where measured atomic form factors are actually used and not Form factors calulated by the Thomas-Fermi-Moliere Model (Z>4).

Coherent Bremsstrahlung

The above equations represent the physics of incoherent bremsstrahlung production.

http://137.99.79.133/halld/tagger/references/inelasticBrems-94.pdf

Radiation Length (Xo)

Radiation Length[math] (X_0)[/math]

The distance an electron travels through matter until loosing [math]\frac{1}{e}[/math] of its energy due to radiation [math]\left ( \frac{dE}{dx} \right )_{rad}[/math].

in the high energy limit where [math]\left ( \frac{dE}{dx} \right )_{col}[/math] can be ignored [math]( E \gt E_C )[/math]

[math]\frac{dE}{dx} = NE_0 \Phi_{rad} \Rightarrow \int_{E_0}^{E} \frac{dE}{E} = -\int_0^X N \Phi_{rad} dx[/math]

[math]\Rightarrow \ln(\frac{E}{E_0}) =-N \Phi_{rad}X[/math]

or

[math]E = E_0 e^{-N \Phi_{rad}X} = E_0 e^{-\frac{X}{X_0}}[/math]

where

[math]X_0 \equiv \frac{1}{N \Phi_{rad}}[/math] = Radiation Length of a given material

ie:

if [math] X = X_0[/math] Then [math]E=\frac{1}{e} E_0[/math] = Energy of electron after traveling a distance of [math]X_0[/math] through the material

Table of Radiation Lengths for several materials
Material	[math]X_0[/math] (cm)
Air	30,050
Al	8.9
Cu	1.43
Fe	1.76
H2O	36.1
NaI	2.59
Pb	0.56
Polystyrene	42.9
Scintillators	42.2

If we have complete screening [math] (\gamma=0)[/math]

Then [math]\frac{1}{X_0} = N \Phi_{rad} = 4 \alpha r_e^2 \frac{N_A}{A} \left \{ Z^2 \left [ L_{rad} - f(Z)\right ] + ZL_{rad}^{\prime}\right \}[/math]

= [math]\frac{Z^2 \left [ L_{rad} - f(Z)\right ] + ZL_{rad}^{\prime}}{716.408 \frac{g}{cm^2}A}[/math]

where

[math]L_{rad} \equiv \frac{1}{4} [\phi_1(\gamma=0) - \frac{4}{3} \ln(Z)] = \left \{ {1 + \int_0^{m_e} [ 1-\frac{F(q)}{Z}]^2 \frac{dq}{q} \;\;\; Z\le4\atop \ln(184.15 Z^{-1/3} \;\;\; Z\gt 4} \right . [/math]= radiation logarithm for elastic Atomic scattering

[math]L_{rad}^{\prime} \equiv \frac{1}{4} [ \phi_2(\gamma=0) - \frac{8}{3}\ln Z]= \left \{ {1 + \frac{1}{2}\int_0^{m_e} \frac{G_2^{inel}(t)}{Z}\frac{dt}{t} \;\;\; Z\le4\atop \ln(1194 Z^{-2/3} \;\;\; Z\gt 4} \right .[/math] = radiation logarithm for inelastic Atomic scattering

[math]f(Z) = \alpha^2 Z^2 \left [ \frac{1}{1+\alpha^2 Z^2} + 0.20206 - 0.0369 \alpha^2 Z^2 + 0.0083 \alpha^4 Z^4 -0.002 \alpha^6 Z^6 \right ][/math] :Z < 92

Quick [math]X_0[/math] Estimates

[math] X_0 = \frac{716.4 \left ( \frac{g}{cm^2} \right ) A }{Z(Z+1) \ln \left ( \frac{287}{\sqrt{Z}} \right )}[/math]

Examples of Radiation length

[math]\frac{1}{e} = \frac{1}{2.72} \sim \frac{1}{3}[/math]

an electron has lost 1/3 of its original energy after traveling 1 radiation length (1 [math]X_0[/math]) through the material

[math]\frac{1}{e^2} \sim \frac{1}{7}[/math]

an electron has lost 1/7 of its original energy after traveling 2 radiation lengths (2 [math]X_0[/math]) through the material

[math]\frac{1}{e^3} \sim \frac{1}{20}[/math]

an electron has lost 1/20 of its original energy after traveling 3 radiation lengths (3 [math]X_0[/math]) through the material

After 2.3 radiation lengths the electron energy is down by a factor of 10 from its original value.

Bremsstrahlung in GEANT 4

GEANT4 uses an energy cut off [math](T_c, k_c)[/math] to decide whether to use a continuous energy loss algorithm (msc, Bethe-Bloch, soft photons) or to generate a secondary particle (photon) and use Bremsstrahliung.

[math]T_C[/math] = incident particle K.E. cutof = secondary particle production threshold

[math]k_c[/math] = photon energy cutoff below which photons are treated as continuous energy loss.

if [math]E_{secondary}\lt T_C[/math] then no photon is created and the effect of the soft photon reaction is treated as a continuous energy loss via

[math]E_{loss}^{Brem} (Z,T,k) = \int_0^{k_c} \left ( \frac{ d \sigma(z,T,k)}{dk}\right ) k dk[/math] = continuous energy loss via "soft" photon emission

[math]\frac{ d \sigma(Z,T,k)}{dk}[/math] = cross sections parametrerized by the Evaluated Electrons Data Library (EEDL)

reference: J. Tuli, "Evaluated Nuclear Structure Data File", BNL-NCS - 51655 -Rev 87, 1987 from Brookhaven Nat. Lab

see National Nuclear Data Center:

Note

Soft photons are photons created in the scattering process which have less energy than the energy of the particles participating in the interaction. Soft photon are not energtic enough to be detected.

To improve simulation speed though, GEANT 4 actually uses a fit to the above cross sections such that

[math]E_{loss}^{Brem} (Z,T,k) = (2 - C_{th}Z^{1/4}) \frac{Z(Z+\epsilon_{\ell})(T+m)^2}{T+2m} \left [ \frac{k_C}{T}\right ]^{\beta} \frac{a+b\frac{T}{T_{\ell m}}}{1+c \frac{T}{T_{\ell m}}} \frac{f_{\ell}}{N_a}[/math]

where

[math]m[/math] = electron mass

[math]T[/math] = kinetic energy of incident particle

[math]N_a[/math] = Avagadros number

[math]\epsilon , \beta, C_{th}, a, b, c[/math] = constants

[math]f_{\ell}[/math] = polynomial (in log(T) ) chosen to fit the data

if [math]E_{secondary}\gt T_C[/math] then a photon is created and tracked

The energy of the emitted photon is determine by sampling a probability distribution from

S. Seltzer and M. Berger, Atomic Data & Nucle. Data tables, vol 35 (1986) pg 345-418

and

the angular distribution ([math]\cos(\theta)[/math]) is sampled according to

E. Acosta, Appl. Phys. Letter, vol 80 # 17 (2002) pg 3228-3230

Note

• The MC program PENELOPE was used to generate the energy distributions that are sampled
• GEANT4 uses a modified version of base equations for [math]e^+e^-[/math] bremsstrahlung with model corrections for [math]e^+[/math]

LPM effect

There is also a correction kown as the Landau Pomeranchuk Migdal (LPM) effect which corrects for multiple scattering experiences by the electron during the scattering which causes the emission of a photon.

Bragg's Rule for compound materials

The radiation length for compounds and mixtures is determined by parallel weighting (resistors in parallel)

[math]\frac{1}{L_{rad}} = \omega_1 \left ( \frac{1}{L_{rad}} \right )_1 + \omega_2 \left ( \frac{1}{L_{rad}} \right )_2[/math]

where

[math]\omega_1[/math] = fraction , by wieght, of each element in the mixture/compound.

[math]= \frac{a_i A_i}{A_m}[/math]

[math]a_1[/math] = # of atoms of element "i"

[math]A_i[/math] = atomic # of element "i"

[math]A_m = \sum a_i A_i[/math] = effective atomic mass of the compound/mixture

Photo-electric effect

The photo-electric effect identifies the physics process by which bound electrons in an atom are liberated by an interaction with an incident photon.

[math]E_f = E-E_B = h \nu - E_B[/math]

where

[math]h\nu[/math] = incident photon energy

[math]E_B[/math] = electron binding energy

Moseley's Law

Moseley's law approximates the binding energies of electrons in atoms as

[math]E_B = 13.605 \frac{\left ( Z-k_s \right )^2 }{n^2}[/math] (eV)

X-ray electron shells are labeled K,L,M

Shell	n	Spect. Notation (low E)	Spect. Notation (High E)	k_s
K	1	[math]1S_0[/math]		3
L	2	[math]2P_{3/2} , 2P_{1/2}[/math]	3P{3/2}	5

Example

Binding Energies for Argon (A=18) "Chemical Rubber Company Handbook of Chemistry and Physics", CRC press. Boca Raton FL, 81st ed, 2000.

Shell	n	Spect. Notation	Binding Energy (eV)
			Measured	GEANT4	Moseley
[math]K[/math]	1	[math]1S[/math]	3218	3178	3061
[math]L_{I}[/math]	2	[math]2S[/math]	328	313.5	575
[math]L_{II}[/math]	2	[math]2P_{1/2}[/math]	251	247	575
[math]L_{III}[/math]	2	[math]2P_{3/2}[/math]	248.4	247	575

Binding energies for a few common elements

Element	Binding Energy (eV)
	n=1	n=2		n=3
B	201	14.2	8.3
C	298	17.9	11.4
N	450	26	15
O	548	33	13.6
Na	1083	71	38	5.2
Mg	1313	94	55	7.7
Al	1573	126	81	11	6
Si	1854	157	107	15	8.2
P	2167	195	141	20	10.5
S	2490	236	172	21.3	10.4
Cl	2844	279	210	25	13
K	3615	386	303	41	25

Photo-electric cross section

the most general expression

[math]\frac{d \sigma}{d \Omega} = 32 \frac{e^2}{4 \pi \hbar c} | \vec{k}^{\prime} | \frac{\hbar}{mc} \frac{c}{\omega} \left ( \frac{z}{a_o} \right )^5 \frac{ \left ( \hat{\epsilon} \cdot \vec{k}^{\prime} \right ) ^2}{ \left [ \frac{z^2}{a_0^2} + q^2 \right ]^4 } [/math]

where

[math]\vec{k}^{\prime} = \frac{\vec{p}}{h}[/math] = scattered electron wave number [[math]\frac{1}{m}[/math] ]

[math]\omega = c | \vec{k} |[/math] = incident photon wave frequency

[math]a_o = \frac{\hbar^2}{(mc)^2}[/math]

[math]\hat{\epsilon}[/math] = incident photon polarization

[math]\vec{q} = \vec{k} - \vec{k}^{\prime}[/math] = momentum given to the atom divided by Plank's constant (h)

if the electron's K.E. after emission is larger than its binding energy

then

[math]k^{\prime} \approx \left ( \frac{2m \omega}{\hbar} \right )^{1/2}[/math]

[math]a_0 = \frac{r_0}{\alpha^2}[/math]

[math]\hat{\epsilon} \cdot {\vec{k}}^{\prime} = k^{\prime} \sin(\theta) \cos(\phi)[/math]

[math]\Rightarrow[/math]

[math]\frac{d \sigma}{d \Omega} = \alpha^4 r_0^2 Z^5 \left ( \frac{mc^2}{\hbar \omega}\right)^{7/2} \frac{4 \sqrt{2} \sin^2(\theta) \cos^2(\phi)}{\left [ 1 - \frac{v}{c}\cos(\theta)\right ]^4} [/math]

For K shell emmission

[math]\sigma = 4 \sqrt{2} \frac{8 \pi r_o^2}{3} \alpha^4 Z^5 \left( \frac{mc^2}{\hbar \omega}\right)^{7/2}[/math]

at higher energies [math](\hbar \omega \gg mc^2 )[/math] (the ultra-relativistic limit

[math]\sigma = \frac{3}{2} \frac{8 \pi r_o^2}{3} \alpha^4 Z^5 \left( \frac{mc^2}{\hbar \omega}\right)[/math]

References

http://physics.nist.gov/PhysRefData/Xcom/html/xcom1.html

http://www-amdis.iaea.org/LANL/

http://www.nist.gov/pml/data/ionization/index.cfm

Mass Attenuation Coefficient

The mass attenuation coefficient [math](\frac{\mu}{\rho})[/math] is used to describe the attenutation of a photon interacting with matter via the photo-electric effect ( absorption), coherent scattering (Rayleigh), incoherent scattering (Compton), or pair production.

[math]\mu[/math] = linear photo-electric attenutaion

[math]\rho[/math] = density of the material

[math]\frac{\mu}{\rho} = \frac{\sigma_{PE}}{amu}[/math]

Eample

Below is an example of the mass atenuation coefficeint as a function of the incident photon energy

a 10 keV photon (0.01 MeV) will have [math]\frac{\mu}{\rho} = 1 \frac{cm^2}{g}[/math] when traveling through water [math](\rho = 1 \frac{g}{cm^3})[/math]

[math]\Rightarrow \mu = 1 \frac{cm^2}{g} \rho = 1 \frac{1}{cm}[/math] = attenuation coefficient

[math] I = I_0 e^{-\mu x}[/math] = intensity of light

if [math]I= \frac{I_0}{2}[/math]

[math]\Rightarrow x = \lambda_{1/2}[/math] = half length = [math]- \frac{1}{\mu} \ln (\frac{1}{2})[/math] = 0.69 cm

This means that 1/2 of the photons impinging on water get absorbed by the water atoms after a depth of 0.69 cm.

Scaling

Sometimes when [math]\frac{\mu}{\rho}[/math] is not available for your material you can scale a [math]\frac{\mu}{\rho}[/math] of a material with similar atomic number using the equation

[math]\left ( \frac{\mu}{\rho} \right)_{unknown} = \left ( \frac{\mu}{\rho} \right)_{known} \left [ \frac{Z^n}{A \rho}\right][/math]

where the coefficient[math] n[/math] varies with the photon energy from 4 [math]\rightarrow[/math] 5 according to:

GEANT4

GEANT4 uses a parameterization of photon absorption cross sections to determine the mean free path, atomic shell data to determine the ejected electron energy, and the k-shell angular distribution to determine the direction of the ejected electron.

The fit to the photoabsorption cross sections

The photoabsorption cross section is parametrized according to

[math]\sigma(Z,E_{\gamma}) = \frac{a(Z,E_{\gamma})}{E_{\gamma}} + \frac{b(Z,E_{\gamma})}{E^2_{\gamma}} + \frac{c(Z,E_{\gamma})}{E^3_{\gamma}} + \frac{d(Z,E_{\gamma})}{E^4_{\gamma}}[/math]

where

[math]a(Z,E_{\gamma}) ,\; b(Z,E_{\gamma}) ,\; c(Z,E_{\gamma}), \;d(Z,E_{\gamma})[/math] are determined by a least squares fit to the data as outlined in

F. Biggs & R. Lighthill, Sandia Lab Preprint, SAND 87-0070 (1990)

File:Biggs Lighthill SandiaPreprint 87-0070.pdf

You select [math]E_{\gamma}[/math] by sampling from a distribution generated by the above cross section.

The mean free path ([math]\lambda[/math]) of the photon through the material is given by

[math]\lambda(E_{\gamma}) = \frac{1}{\sum_i N_i \sigma(Z_i,E_{\gamma})}[/math]

where

[math]N_i = \frac{\mbox{number of Atoms of} \quad i^{th} \quad\mbox{element } \quad Z_i \quad \mbox{in the material}}{\mbox{Volume}}[/math]

K.E. of ejected electron

Given that a photo-electric event happens then the energy of the ejected electron is given by

[math]T_{p.e.} = E_{\gamma}-B_{shell}(Z_i)[/math]

where

[math]E_{\gamma}[/math] = energy of the incident photon

[math]B_{shell}(Z_i)[/math] = electron shell energy from the closest available atomic shell as tabulated in data/G4EMLOW/fluor/binding.dat

The shell is selected according to the shell cross sections

Electron direction

The ejected electron is chosen by an angle according to the Souter-Gavrila distribution (Gavrila_M._Phys.Rev._vol113_1959_pg514) in the "standard" package such that

[math]\cos(\theta) = \frac{rnd + \beta}{rnd\times \beta +1}[/math]

where rnd is a random number chosen such that

[math]\frac{1-\cos^2(\theta)}{(1-\beta \cos(\theta))^2} \times \left [ 1 + b(1-\cos(\theta) \right ] \lt rnd \times \left \{ { \gamma^2(1+b(1-\beta)) \quad \gamma \lt 2 \atop \gamma^2(1+b(1+\beta) ) \quad \mbox{otherwise} } \right .[/math]

[math]b = \frac{\gamma (\gamma -1) ( \gamma -2)}{2}[/math]

[math]\gamma = 1+ \frac{\mbox{K.E.}_{e^-}}{m_ec^2}[/math]

G4PhotoElectricEffect

This model will generate an ionized electron which is about the same as the incident photon energy. Don't use this one if your simulation is sensitive to atomic energy levels (ie; looking at keV energy effects). This should be O.K. if you are just interested in attenuating photons.

G4LowEnergyPhotoElectric

This process will generate ionized electrons for each possible electron binding energy which is less than the incident photon energy. It should be cross section weighted.

This model seems to break when [math]E_{\gamma} \le[/math] 100 keV (GEANT4 version 4.8)

PAI Model

PhotoAbsorption Ionizaton (PAI) Model

The PAI model uses a least squares fit of a 4th order polynomial in [math]\frac{1}{\omega}[/math] to the experimental photoabsorption data for the cross section such than

[math]\sigma(\omega) = \sum_i^4 \frac{a_k(E)}{\omega^k}[/math]

where

[math]a_k(E)[/math] = fit coefficent for energy bin [math]E[/math]

[math]\omega[/math] = energy transfered in the ionization collision

Compton Scattering

Compton scattering is like the photo-electric effect except the photon isn't absorbed but scattered by atomic electrons.

"Ideal" compton scattering is described in terms of free electrons.

The collision is elastic

[math]\lambda^{\prime} = \lambda + \lambda_C (1-\cos(\theta)) = \frac{2 \pi}{\omega^{\prime}} = \frac{ch}{E_{\gamma}^{\prime}} = \frac{12,400 \mbox{Angstroms}}{E_{\gamma}^{\prime}}[/math]

[math]\lambda_C[/math] = electron compton wavelength = [math]\frac{h}{m_ec} = 2.43 \times 10^{-12} m[/math]

[math]E_k = \hbar \omega \frac{\lambda_C}{\lambda} \frac{1- \cos(\theta)}{1 + \frac{\lambda_C}{\lambda} \left (1 - \cos(\theta) \right )}[/math] = electron final kinetic energy

[math]\phi = \cot \left [ \left ( 1+ \frac{\lambda_C}{\lambda}\right ) tan(\frac{\theta}{2}\right ][/math] = ejected electron angle w.r.t original photon direction

Note

[math]\phi_{max} = \frac{\pi}{2}[/math] : No electrons can be backscattered in the compton process.

The photon can backscattered

[math]\theta = \pi[/math] = Max energy transfered to the [math]e^-[/math]

[math]E_k(max) = \frac{2 \hbar \omega \lambda_C}{\lambda + 2 \lambda_C}[/math] = The max energy transfer point corresponds to the "compton" edge

Example

Find [math] E_k(max)[/math] of the compton edge for a given [math]E_{\gamma}[/math].

[math]E_k(max) = \frac{\hbar \omega }{\frac{\lambda}{2 \lambda_C} + 1} = \frac{E_{\gamma} }{\frac{\lambda}{2 \lambda_C} + 1}[/math]

[math]\lambda = \frac{c}{\nu} = \frac{c h}{E_{\gamma}}[/math]

[math]E_k(max) =\frac{E_{\gamma} }{\frac{c h}{2 \lambda_C E_{\gamma}} + 1} =\frac{E_{\gamma} }{\frac{3 \times 10^8 \frac{m}{s} 4.14 \times 10^{-15} \frac{eV}{s}}{2 \times 2.43 \times 10^{-12} m E_{\gamma}} + 1}[/math]

[math]\approx 4 \times 10^{-6} \frac{E_{\gamma}^2}{1 + 4 \times 10^{-6} E_{\gamma}}[/math]

If [math]E_{\gamma}[/math] = 8 keV

Then [math]E_k(max) \approx 256[/math] eV = max energy lost by photon and given to electron

Cross Section

The Klein-Nishina formula (Oskar Klein & Yoshio Nashina, Z. fur Phys., vol 52 (1929), pg 853 ) is given as

[math]\frac{d \sigma}{d \Omega} = \frac{r_e^2}{2} \frac{1 + \cos^2(\theta) + \frac{\xi^2 \left [ 1+ \cos(\theta) \right ]^2}{1 + \xi \left( 1+ \cos(\theta) \right)}}{\left[ 1+ \xi (1-\cos(\theta) ) \right ]^2}[/math]

where

[math]\xi = \frac{h \nu}{m_e c^2} = \frac{E_{\gamma}}{E_0^{e^-}} = \frac{E_{\gamma}}{0.511 MeV} \approx 2\frac{E_{\gamma}}{MeV}[/math]

Note

The above cross section is for a free electron. Multiple by [math]Z[/math] (the number of electrons in the target) to get the atomic cross section.

After integrating over [math]d \Omega[/math]

[math]\sigma_{compt} = 2 \pi r_e^2 \left \{ \frac{1+\xi}{\xi^2} \left [ \frac{2(1+\xi)}{1 + 2\xi} - \frac{1}{\xi} \ln(1+2 \xi) \right ]\right \}[/math]

Energy Distribution

The compton electron energy distribution can be evaluated from the differential cross section below

[math]\frac{d \sigma}{d E^{e^-}} = \frac{\pi r_e^2}{m_e c^2 \xi^2} \left [ 2 + \frac{s^2}{\xi^2 (1-s)^2} + \frac{s}{1-s} \left ( s - \frac{2}{\xi}\right )\right ][/math]

where

[math]s = \frac{E^{e^-}}{h \nu} = \frac{E^{e^-}}{E_{\gamma}}[/math]

[math]\xi \approx 2 E_{\gamma}[/math]

[math]r_e^2 = 0.794[/math] barns

[math]m_e c^2 = 0.511[/math] MeV

GEANT 4

GEANT 4 parametrized the Compton cross section to reproduce the data down to 10 keV using the expression

[math]\sigma(Z,E_{\gamma}) = \left [ P_1(Z) \frac{\log(1+2 \xi)}{\xi} + \frac{P_2(Z) + P_3(Z) \xi + P_4(Z) \xi^2}{1 + a \xi + b \xi^2 + c \xi^3} \right ][/math]

[math]P_i(Z) = d_i Z + e_i Z^2 + f_i Z^3[/math]

[math]1 \le Z \le 100[/math]

[math] a,b,c, d_i, e_i, f_i[/math] are determined from fit

The data used in the fit may be found in

Hubbell, Grimm, & Overbo, J. Phys. Chem. Ref. Data 9, (1980) pg 1023

H. Storm, Nucl. Data Tables, A7 (1970) pg 565

In addition to the default and low energy models which come with GEANT4 (as was available with the Photo Electric effect), there is also a model called "G4LECS" which may be installed.

Models

a.) G4ComptonScattering: listed as "compt" in the process name. No Rayleigh scattering in the model.

b.) G4LowEnergyCompton: Process name is "LowEnCompton" in the tracking code. It has errors in the treatment of Rayleigh scattering and does not account for doppler broadening (the effect of bound electron momentum on the scattered particle energies).

c.) G4LECS: Bound electron effects are corrected for on an :shell-by-shell" basis. Rayleigh scattering is modeled using the coherent scattering cross section and form factor data. The Doppler broadening effect is included ( a result of the compton telescope simulation work).

Note

Thomson & Rayleigh scattering are classical processes related to Compton scattering. Klein-Nishina formula reduces to the Thomson cross section at low energies such that [math]\sigma_{Thompson} = \frac{8 \pi}{3} r_e^2[/math]. Thomson scattering produces polarized light because at these low non-relativistic energies the particle that absorbs the photon emits it in a direction perpendicular to its motion, that motion is the results of sees the oscillating E & M wave from the incident photon. Rayleigh scattering (why our sky is blue) is photon scattering from an atom as a whole, coherent scattering. No energy is transfered to the Medium in either case, [math]\gamma[/math] only changes direction. Rayleigh scattering is the elastic scattering of the photon from a particle that is smaller than the wavelength of the light. Mei theory is used to describe elastic scattering from particles that are larger than the wavelength of the incident photon.

Pair Production

Pair production is similar to the Bremsstrahlung process.

Remember, in Bremsstrahlung the incident charged particle interacts with the [math]\vec{E}[/math] of the Nucleus (or shell electron)

In pair production a photon interacts with the [math]\vec{E}[/math] of the Nucleus.

when the recoil of the atom is taken into account

[math]E_{threshold} = 2 m_e(1+\frac{m_e}{M_A})[/math] = Threshold energy for pair production from an atom of mass [math]M_A[/math]

Note

You can also have photon-electron pair production analogous to electron-electron bremsstrahlung production.

Pair Production Cross Section

The pair production cross section is given by Equation 6.35 in (Bethe, Phys. Rev., vol. 93 (1964) pg 768)

at small angles

A version which assumes small angles is given in Eq 7.35 of the same reference as the triple differential cross section:

[math]\frac{d \sigma}{d \epsilon_1 d \theta_1 d \theta_2} = 8 \left ( \frac{\pi a}{\sinh (\pi a)} \right )^2 \frac{a^2}{2 \pi} \frac{e^2}{\hbar c} \left ( \frac{\hbar}{m_e c }\right )^2 \frac{\epsilon_1 \epsilon_2}{k^3} \theta_1 \theta_2 [/math]

[math]\times \left \{ \frac{V^2(x)}{q^4} \left [ k^2 (u^2 + v^2) \xi \eta - 2 \epsilon_1 \epsilon_2 (u^2 \xi^2 + v^2 \eta^2 ) + 2 (\epsilon_1^2 + \epsilon_2^2)uv \xi \eta cos(\phi) \right ] \right . [/math]

[math]\left . + a^2W^2(x) \xi^2 \eta^2 \left [ k^2(1 - (u^2+v^2)\xi \eta - 2 \epsilon_1 \epsilon_2 (u^2 \xi^2 + v^2 \eta^2) -2 (\epsilon_1^2 + \epsilon_2^2) u v \xi \eta \cos(\phi)\right ]\right \}[/math]

where

[math]k =[/math] photon momentum/energy

[math]\theta_1[/math] = scattering angle of [math]e^+[/math]

[math]\theta_2[/math] = scattering angle of [math]e^-[/math]

[math]\phi = \phi_1 - \phi_2 = \phi[/math] angle between the [math]e^+[/math] and [math]e^-[/math] pair

[math]\epsilon_1 = \sqrt{p_1^2 + m_e^2}[/math] = Energy of the positron

[math]\epsilon_2 = \sqrt{p_2^2 + m_e^2}[/math] = Energy of the electron

[math]u = \epsilon_1 \theta_1[/math]

[math]v=\epsilon_2 \theta_2[/math]

[math]\xi = \frac{1}{1+u^2}[/math]

[math]\eta= \frac{1}{1+v^2}[/math]

[math]q^2 = u^2 + v^2 + 2 u v \cos(\phi)[/math]

[math]x= 1-q^2 \xi \eta[/math]

[math]V(x) = 1 + \frac{a^2}{(1!)^2} + \frac{a^2 (1+a^2) x^2}{(2!)^2} + \frac{a^2 (1+a^2)(2^2+a^2)x^4 x^2}{(3!)^2} + \cdots[/math]

[math]W(x) = \frac{1}{a^2} \frac{d V(x)}{d x}[/math]

[math]a = \frac{Ze^2}{\hbar c}[/math]

Note

The above equations for the differential cross section are using "natural" units where [math]c \equiv 1[/math]

Davies' version integrates over all angles

Davies published a version which has been integrated over angles and includes some screening effects ( see Eq 35):

[math]\frac{d \sigma}{d \epsilon_1} = 2 a^2 \frac{e^2}{\hbar c} \left ( \frac{\hbar}{m_e c }\right )^2 \frac{\epsilon_1^2 +\epsilon_2^2 + + \frac{2}{3} \epsilon_1 \epsilon_2 }{k^2} \left [ 2 \log \left (\frac{2\epsilon_1 \epsilon_2}{k^2} \right ) - 1 - 2 f(Z)\right ][/math]

[math]= 4 Z^2 \alpha r_2^2 \frac{\epsilon_1^2 +\epsilon_2^2 + + \frac{2}{3} \epsilon_1 +\epsilon_2 }{( h \nu)^3} \left [ 2 \log \left (\frac{2\epsilon_1 \epsilon_2}{h \nu m_e c^2} \right ) - 1 - 2 f(Z)\right ][/math]

where

[math]f(Z) = a^2 \sum_1^{\infty} \frac{1}{\nu (Z^2 +a^2)} \sim \frac{1}{1+a^2} + 0.20206 - 0.0369 a^2 + 0.0083 a^4 - 0.002 a^6[/math]

If you integrate over all positron ([math]\epsilon_1[/math] ) energies you get Eq. 44 (no screening)

[math]\sigma_{e^+e^-} = 4 Z^2 \alpha r_e^2 \left [ \frac{7}{9} \right ( \ln(\frac{2 h \nu}{m_e c^2}) -f(Z) \left ) - \frac{763}{378} \right ][/math]

and Eq. 45 (complete screening)

[math]\sigma_{e^+e^-} = 4 Z^2 \alpha r_e^2 \left [ \frac{7}{9} \right ( \ln(\frac{183}{Z^{\frac{1}{3}}}) -f(Z) \left ) - \frac{7}{378} \right ][/math]

Davies expressions were shown to work well at high energies ([math]E_{\gamma} \gt 88[/math] MeV)

Overbo's low energy Cross sections

At low energies ( [math]E_\gamma \lt 5[/math] MeV), Overbo published an exact calculation in the case that the Atomic field is unscreened. Overbo then provided a fit to the results of his calculation which he claims is valid to within 0.1% for the energy range [math](3 MeV \lt E_{\gamma} \lt 5 MeV)[/math]. The fit is given in Eq. 7.1 of his paper as

[math]\sigma_{e^+e^-} = \sigma_B \left ( 1 + a + \frac{b}{k-2}\right )[/math]

where

[math]a= -0.44 (\alpha Z)^2 - 0.07 (\alpha Z)^4[/math]

[math]b= 5.06 (\alpha Z)^2 - 2.1 (\alpha Z)^4[/math]

[math]\sigma_B = \alpha Z^2 r_e^2 \frac{2 \pi}{3} \left ( \frac{k-2}{k} \right ) ^3 \left [ 1 + \frac{\epsilon}{2} + \frac{23 \epsilon^2}{40} + \frac{11 \epsilon^3}{60} + \frac{29\epsilon^4}{960} \right ]=[/math] Low Energy unscreened Born approximation total cross section for pair production

[math] k = \frac{h \nu}{m_e c^2} = \frac{E_{\gamma}}{0.511 MeV}[/math] = incident photon energy in units of the electron rest mass energy

[math]\epsilon \equiv \frac{2k -4}{2+k+2\sqrt{2k}}[/math]

Intermediate Energy Cross sections

For [math]5 MeV \lt E_{\gamma} \lt 80 MeV[/math] the Gradstein semi-ephirical formula is used from G. White Gradstein, Natl. Bur. Standard., Circ 583 (1957) pg 1.

[math]\sigma = \sigma_{BH} - \Delta_e + \frac{b^2}{k} \ln(k -0.57)[/math]

where

[math]\Delta_e[/math] = empirical constant = 4.02 barns for Pb

[math]b^2[/math] = empirical constant = 16.8 barns for Pb

[math]\sigma_{BH}[/math] = Simulations_of_Particle_Interactions_with_Matter#Bremsstrahlung Bethe-Heitler cross section

Triplet production

Triplet Production

identifies photon-electron pair production. The recoiling electron track adds to the two [math]e^+e^-[/math] tracks making three total particle tracks (kind of like pair production ionization).

A description for how to calculate the cross section for this process is illustrated for 1[math]0 \lt E_{\gamma} \lt 20 MeV[/math] in L.E. Wright, Phys. Rev. C 36 (1987) pg 582. Unfortunately, analytic expression is not given but one could construct tables of [math]Tq(92)[/math] and [math]Tq(1)[/math] in equation 65 of L.E. Wright's paper.

An example for [math]E_{\gamma} =6 MeV[/math] may be found in Sud & Vargus, Phys. Rev. A49 (1994) pg 4624.

GEANT4 Pair production

GEANT4 uses the pair production cross section given in Tsai, Rev. Mod. Phys, vol 46 (1974) pg 815.

[math]\frac{d \sigma}{d \epsilon} = Z(Z+ \eta) \alpha r_e^2 \left \{ \left [ \epsilon^2 +(1- \epsilon)^2 (\phi_1 - 4f(Z) ) \right ] + \frac{2}{3} \epsilon(1-\epsilon) (\phi_2 - 4f(Z) )\right \}[/math]

where

[math]E_{\gamma} =[/math] energy of incident photon

[math]E_{e^-} =[/math] KE of create electron

[math]\epsilon = \frac{E_{e^-} +m_ec^2}{ E_{\gamma}} =[/math] fraction of [math]E_{\gamma}[/math] taken away by [math]e^-[/math]

[math]\eta=[/math] triplet production correction

[math]f(Z) =[/math] high energy coulomb correction from Davies above

[math]\phi_1[/math] & [math]\phi_2[/math] = electron screening functions

The formula GEANT4 uses may also be found on pg 541 in J. Bono , Radiation Physics Chemistry, vol 44 (1994) pg 531

[math]\frac{d \sigma}{d\epsilon} = \frac{2}{3} Z(Z+ \eta) \alpha r_e^2 C_r \left [ 2(\frac{1}{2} - \epsilon)^2 \phi_1(\epsilon) + \phi_2(\epsilon) \right ] [/math]

where

[math]\phi_1(\epsilon) = g_1(b) + g_0(\kappa)[/math]

[math]\phi_2(\epsilon) = g_2(b) + g_0(\kappa)[/math]

[math]g_1(b) = \frac{2}{3} - 2 \ln(1+b^2) - 6b \tan^{-1}(\frac{1}{b} - b^2 \left [ 4 -4b\tan^{-1}(\frac{1}{b} -3 \ln(1 + \frac{1}{b^2}\right][/math]

[math]g_2(b) = \frac{11}{6} - 2 \ln(1+b^2) - 3b \tan^{-1}(\frac{1}{b} - \frac{b^2}{2} \left [ 4 -4b\tan^{-1}(\frac{1}{b} -3 \ln(1 + \frac{1}{b^2}\right][/math]

[math]g_0(\kappa) =4 \ln ( \frac{R m_e c}{\hbar}) + 4f(Z) + F_0(\kappa,Z)[/math]

[math]F_0(\kappa,Z) = \left [ -0.1774 - 12.10 \alpha Z + 11.18 (\alpha Z)^2 \right ] \sqrt{\frac{2}{\kappa}} + \left [ 8.523 + 73.26 \alpha Z - 44.41(\alpha Z)^2 \right ] \frac{2}{\kappa}[/math]

[math]- \left [ 13.52 + 121.1 \alpha Z - 96.41 (\alpha Z)^2 \right ] \left ( \frac{2}{\kappa} \right)^{2/3} + \left [ 8.946 + 62.05 \alpha Z - 63.41(\alpha Z)^2 \right ] \left ( \frac{2}{\kappa} \right )^2[/math]= low energy coulomb correction

[math]R[/math] = screening radius (adjustable parameter)

[math]\frac{\hbar}{m_ec} = 3.8616 \times 10^{-13} m[/math] = Compton wavelength

[math]b = \frac{Rm_e c}{\hbar} \frac{1}{2\kappa} \frac{1}{\epsilon(1-\epsilon)}[/math]

[math]\kappa = \frac{E_{\gamma}}{m_e c^2}[/math]

An older simulation description with graphs of the cross-sections may be found below.

File:Bigg Lighthill conversion 1Mev-100MeV SandiaPreprint SC-RR-68-619.pdf

Below is the review of Modern Physics article basically summarizing all of the physics for pair production up to 1969

File:RevModPhys PairPoduction 1969 MotzOlsonKoch.pdf

Contributions as function of Z

The plot below shows the contributions of the three photon absorption physics processes as a function of the incident photon energy and the Z of the target material. At low energy (keV), the photo-electric effect dominant while at high energies (> 1 MeV) pair production starts to dominate. Compton scattering dominates in the intermediate energy region.

Hadronic Interactions

Proton Bremsstrahlung

[math]\sigma_{class}|_{90^o} = 2.1\times 10^{-31} cm^2/sterad[/math] = cross section for dipole radiation emitted at 90 degrees with respect to incident beam of particles scattered in a Coulomb field.

File:ProtonBrem Drell Huang PhysRev v99 n3 1955 pg686.pdf

Pluto event generator

A ROOT based Hadronic Simulation package based on Pluto

I installed Pluto V 5.14.1 on inca

I needed to set the environmental variables under tcsh

setenv ROOTSYS ~/src/ROOT/root
setenv PATH ${PATH}:${ROOTSYS}/bin
setenv LD_LIBRARY_PATH $ROOTSYS/lib

There is a subdirectory called "macros"

cd macros

Go to that subdirectory and type root, this will run the contents of the file "rootlogin.C"

cd macros

inca:~/src/Pluto/pluto_v5.14.1/macros> root
 *******************************************
 *                                         *
 *        W E L C O M E  to  R O O T       *
 *                                         *
 *   Version   5.17/03    30 August 2007   *
 *                                         *
 *  You are welcome to visit our Web site  *
 *          http://root.cern.ch            *
 *                                         *
 *******************************************
Compiled on 5 September 2007 for linux with thread support.
CINT/ROOT C/C++ Interpreter version 5.16.24, July 26, 2007
Type ? for help. Commands must be C++ statements.
Enclose multiple statements between { }.
 *********************************************************
 * The Pluto event generator                              
 * (C) HADES collaboration and all contributing AUTHORS   
 * www-hades.gsi.de/computing/pluto/html/PlutoIndex.html  
 * Version: 5.14.1
 * Compiled on 10 December 2008
 *********************************************************
Shared library Pluto.so loaded

to run a pp elastic model type

root [0] .x pp_elastic.C 

a root ntuple is generate called "pp_elastic.root"

you can then analyze the data in the root file with

data->MakeClass();

the above command within root generates an analysis skeleton program.

using t.Show you can see the structure of the events within the ntuple. A few functions are also stored in the root tree which you can use. You can use the root file event to create an input file which GEANT4 can then use as its event generator. GEANT4 then reads the events in and propagates them through your geometry.

Neutron Interactions

Name	Energy
Cold Neutron	micro eV
Thermal	[math]\sim \frac{1}{40}[/math] eV
epithermal	[math] \frac{1}{40} eV \rightarrow 100 keV[/math]
fast	[math]100 keV \rightarrow 100 MeV[/math]
high energy	[math] \gt 100 MeV[/math]

Note: Interaction length for neutrons is ~[math]10^{-13}[/math] .
Neutrons are even better than photons for penetrating matter.

Elastic scattering

File:Elastic scattering from Nuclei.jpg

[math]v_{CM} = \frac{m_n v_L + M(0)}{m_n + M} = \frac{v_0}{1 + \frac{M}{m_n}} = \frac{v_0}{1+A} =[/math] velocity of CM frame

[math]{v_L}^' = [/math] Magnitude of Neutron velocity in CM frame before and after collision
[math]= v_c - v_{CM} = v_0 -\frac{v_0}{1+A} = \frac{(1+A)-1}{1+A} v_0 = \frac{A}{1+A} v_0[/math]

[math] v = [/math] Magnitude of Nucleus velocity in CM frame before and after collision
[math]= v_{CM} = \frac{v_0}{1+A}[/math]

Note: In elastic collision only the particles direction changes.

[math]\vec{v}_L = {\vec{v}_L}^' + \vec{v}_{CM}[/math]

File:Rule of cosines.jpg

[math]c^2 = a^2 + b^2 - 2abcos \theta[/math]

[math](v_L)^2 = ({v_L}^')^2 + (v_{CM})^2 - 2 v_{CM} {v_L}^' cos(\pi - {\theta}_{CM})=[/math]

[math]= ({v_L}^')^2 + (V)^2 - 2 V {v_L}^' cos(\pi - {\theta}_{CM})=[/math]

where

[math]({v_L}^')^2 = (\frac{A}{1+A})^2 {v_0}^2[/math]

[math](V)^2 = (\frac{1}{1+A})^2 {v_0}^2[/math]

After substitution we get following:

[math](\frac{v_L}{v_0})^2 = \frac{A^2 +1 - 2 A cos(\pi - {\theta}_{CM})}{(1+A)^2} = \frac{A^2 +1 + 2 A cos({\theta}_{CM})}{(1+A)^2}[/math]

[math] cos(A+/-B) = cosAcosB -/+ sinAsinB[/math]

[math]\frac{E}{E_0} = \frac{A^2 + 1 + 2Acos({\theta}_{CM})}{(1+A)^2}[/math]

when [math]{\theta}_{CM}=0[/math], [math]E_{max} = E_0[/math].

[math]E_{min} = \frac{(A-1)^2}{(A+1)^2} E_0 = (\frac{A-1}{A+1}) E_0 =[/math] Minimum energy of scattered Neutron in LAB frame.

File:Rule of cosines 1.jpg

[math]({v_L}^')^2 = (v_L)^2 + (v_{CM})^2 - 2 v_{CM} v_L cos(\pi - {\theta}_{CM})=[/math]

[math]= (v_L)^2 + (V)^2 - 2 V v_L cos({\theta}_{L})=[/math]

[math](\frac{Av_0}{1+A})^2 = {v_L}^2 + (\frac{v_0}{1+A})^2 - 2 v_L (\frac{v_0}{1+A}) cos({\theta}_L)[/math]

After substituting [math]v_L[/math]

[math]cos{\theta}_L = [\frac{A^2 + 1 + 2 A cos{\theta}_{CM}}{(1+A)^2} + (\frac{1}{1+A})^2 - (\frac{A}{1+A})^2] \times \frac{(1+A)^2}{2\sqrt{A^2 +1 + 2Acos{\theta}_{CM}}} = [/math]

[math]= \frac{[A^2 +1 + 2Acos{\theta}_{CM} + 1 - A^2]}{2\sqrt{A^2 +1 + 2Acos{\theta}_{CM}}} = \frac{1 + Acos{\theta}_{CM}}{\sqrt{A^2 +1 + 2Acos{\theta}_{CM}}} [/math]

Note: [math] {E_A}^{CM} = \frac{1}{2} M_A V^2 = \frac{1}{2} A m_n (\frac{v_0}{1+A})^2 = \frac{A}{(1+A)^2} \frac{m_n {v_0}^2}{2}= [/math]

[math] = \frac{A}{(1+A)^2}E_0 = [/math] Energy of recoil Nuclei in CM frame.

Conservation of Energy: [math]E_0 = E + E_A[/math]

[math] E_A = E_0 - E = E_0 - \frac{A^2 + 1 + 2Acos{\theta}_{CM}}{(1+A)^2} E_0 = [/math]

[math]\frac{(1+A)^2 - (A^2 +1 + 2Acos{\theta}_{CM})}{(1+A)^2}E_0 =[/math]

Resources

GEANT4 Home Page

ROOT Home page

Fermi Lab Example

NIST Range Tables

X-ray specturm

Installing_GEANT4.9.3_Fsim

Building GEANT4.9.5

TF_GEANT4.9.5

An old version of Installation notes for versions prior to 9.5

Old Install Notes

Visualization Libraries:

OpenGL

DAWN

Coin3D

TF_SPIM_OLD