Tony WeidbergNuclear Physics Lectures1 Applications of Nuclear Physics Fusion –(How the sun works...
-
date post
21-Dec-2015 -
Category
Documents
-
view
218 -
download
0
Transcript of Tony WeidbergNuclear Physics Lectures1 Applications of Nuclear Physics Fusion –(How the sun works...
Tony Weidberg Nuclear Physics Lectures 1
Applications of Nuclear Physics
• Fusion– (How the sun works covered in Astro
lectures)– Fusion reactor
• Radioactive dating– C dating– Rb/Sr age of the Earth
Tony Weidberg Nuclear Physics Lectures 2
Physics of Nuclear Fusion
• All reactions at low energy are suppressed by Coulomb barrier (cf decay).
• Reaction rate: convolution of MB distribution and barrier penetration.
222 1 2
0
(0)( ) ~ exp( )
24
G
G
S EE
E E
Z Z eE mc
c
Tk2
mvexpv
Tk
m2)v(P
B
22
2/3
B
2/1
Tony Weidberg Nuclear Physics Lectures 3
Low Energy Fusion Cross Sections
• Breit-Wigner (no-spin)
• cf decay theory, allow for QM tunnelling through Coulomb barrier
•
4/)EE(k)E(
220
i2
4/)EE(
)/(
mE2)E(
220
i3
)4(c
eZZmc2E;
E
Eexp)E(p
0
2212
GG
Tony Weidberg Nuclear Physics Lectures 4
Cross Sections (Continued)
• Predicts cross section
• Low energy approximation
0i
)]E(Gexp[/
E
EE
exp
4/)EE(m2)E(
G
2200
3
E
Eexp)0(S
E
1)E( G
Tony Weidberg Nuclear Physics Lectures 5
Example C
Theory explains rapid rise at very low energy
Ignores multiple resonances!
Tony Weidberg Nuclear Physics Lectures 6
Fusion Rates
• Consider reaction a+bX (a different from b)– Volume number density a b
– Cross section ab
• Reaction rate/volume )v(vR abba
0
)()()( dvvPvvvv abab
mvdvdEmvE 2
2
1
Tony Weidberg Nuclear Physics Lectures 7
E/EexpE
)0(S
Tk
Eexp
m2
E
Tk
m2dEv G
B2
2/3
B
2/1
0ab
3/ 21/ 2
0
8 1(0) exp[ ( )]
( ) / /
abB
B G
v S dE Em k T
E E k T E E
Maximum rate minimum for
0E
E
2
1
Tk
1
dE
d2/3
0
G
B
Tony Weidberg Nuclear Physics Lectures 8
Fusion Rates
Look at exp[-(E)] Function sharply peaked at E=E0
3/2B
2/1G0 )Tk()E(E
pp reaction
E (KeV)10
6ex
p[-
E)]
Tony Weidberg Nuclear Physics Lectures 9
Fusion Rates
• Most favourable rates for d-t reactions.
• Peak at kBT~ 20 keV
• Why? <v
(v)>
m3s-1
kBT (keV)
Tony Weidberg Nuclear Physics Lectures 10
Fusion Reactors
• Use deuterium + tritium:
– Large energy release– Large cross-section at low energy– Deuterium abundant (0.015% of H).– Breed Tritium in Lithium blanket– .
MeV62.17nHeHH 42
31
21
MeV8.4HeHLin
nHeHMeV46.2Lin42
31
63
42
31
73
Tony Weidberg Nuclear Physics Lectures 11
Fusion Reactors
• Energy out > Energy in
• Lawson criteria (assume kBT=20 keV).– number density D ions : – Cross-section: – Confinement time for plasma: tc
– Energy released per fusion: Efusion
cfusion2
out tEvE
TkE Bin c1319
inout t)sm10(~E/E
Tony Weidberg Nuclear Physics Lectures 12
Magnetic Confinement
• Confine plasma with magnetic fields.– Toroidal field: ions spiral around field
lines.– Poloidal fields: focus ions away from
walls.
• Heating:– RF power accelerates electrons– Current pulse causes further heating.
Tony Weidberg Nuclear Physics Lectures 13
Jet
Tony Weidberg Nuclear Physics Lectures 14
Tony Weidberg Nuclear Physics Lectures 15
MAST
Fusion Progress–Huge strides in physics,
engineering, technology–JET: 16 MW of fusion
power ~ equal to heating power. 21 MJ of fusion energy in one pulse
–Ready to build ITER - the next generation, GigaWatt-scale
–Scaling laws that fit data from existing tokamaks give confidence that ITER/power plants will achieve desired performance
Temperature / 106 K
Fu
sio
n p
rod
uct
p t
(at
m.
sec)
Tony Weidberg Nuclear Physics Lectures 16
AUG JET
ITER
JET
Cross section of present EU D-shape tokamaks compared to the ITER project
Prediction of ITER performancePrediction of ITER performance
Tony Weidberg Nuclear Physics Lectures 17
High Energy neutrons
• Use n to make 3H in Li blanket
• n damage to surrounding support structures ~ 10 dpa/yr
• 2H +7Li n + 2 4He
Tony Weidberg Nuclear Physics Lectures 18
Inertial Confinement Fusion
Very Big Laser
Mirrors
D-T Pellet
Tony Weidberg Nuclear Physics Lectures 19
Inertial Confinement Fusion
Tony Weidberg Nuclear Physics Lectures 20
Radioactive Dating
• C14/C12 for organic matter age of dead trees etc.
• Rb/Sr in rocks age of earth.
Tony Weidberg Nuclear Physics Lectures 21
Carbon Dating• C14 produced by Cosmic rays (mainly
neutrons) at the top of the atmosphere.– n N14 p C14
• C14 mixes in atmosphere and absorbed by plants/trees constant ratio C14 / C12 . Ratio decreases when plant dies. t1/2=5700 years.
• Either– Rate of C14 radioactive decays– Count C14 atoms in sample by Accelerator Mass
Spectrometer.
• Which is better?• Why won’t this work in the future?
Tony Weidberg Nuclear Physics Lectures 22
Carbon Dating Calibration
Tony Weidberg Nuclear Physics Lectures 23
How Old Is The Earth?
• Rb87 Sr87: decay t1/2=4.8 1010 yr
• Assume no initial daughter nuclei get age from ratio of daughter/parent now.
)t(N)t(N)t(N 0p1P1D
)tt(exp()t(N)t(N 010p1P
)t(N
)t(Nln1
t1p
0p
)t(N
)t(N1ln
1t
1p
1D
Tony Weidberg Nuclear Physics Lectures 24
Improved Calculation• Allow for initial daughters to be present.• Need another isotope of the daughter D’ which is stable
and not a product of a radioactive decay chain. • Plot vs straight line fit age and initial ratio.
)t(N)t(N)t(N)t(N 0p0D1P1D
)t(N
)t(N
1D
1D
)t(N
)t(N
1D
1P
)t(N
)t(N)t(N
)t(N
)t(N)t(N
0D
0p0D
1D
1P1D
)t(N
)t(N]1)t[exp(
)t(N
)t(N
)t(N
)t(N
0D
0D
1D
1P
1D
1D
Tony Weidberg Nuclear Physics Lectures 25
Age of Earth
• Rb/Sr method• Stable isotope of
daughter is Sr86
• Fit gives age of earth=4.53 109 years. S
r87/
Sr8
6
Rb87/Sr86
1.0 4.0