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Nuclear reactions
Micro-world Macro-world
Lecture 17
Using the strong nuclear force to produce useful energy
Strong Nuclear Force
• It is very strong– It overcomes the electrical
repulsion between positively charged protons that are only 10-
15m apart.
• It acts over a very short range– It is not felt by nucleons when they
are more than 10-15m apart.
• It is selective– It is felt by neutrons & protons, but
not by electrons
Nuclear “bullets”Protons are repelled by electrical the repulsion force of the positively nucleus. Only protons with KE ofa few MeV or more can get within the range of thestrong nuclear force & produce “nuclear reactions”
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Producing nuclear reactionswith protons (or any other
charged nuclei) is a challenge
Neutron induced nuclear reactions
Neutrons don’t feel the electrical force so even very slow, low-energy neutrons can strike the nucleus & produce “nuclear reactions”
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Low energy neutrons areeffective nuclear “bullets”
Nuclear fission
n + 92U 56Ba + 36Kr + 2n235 142
92
Energy balance in a fission reaction
141Ba +92Kr + 2n
200 MeV KE heat 235U + n
Chain reaction
Use the neutrons produced by onefission to initiate another fissionEnrico Fermi
Requirements for A-bomb
• Fissionable material: 235U or 239Pu
• Critical mass
• Mechanism
Critical Mass
Enriched 235U 50kg
239Pu 10kg
Mcrit
Fissionable Material
Fortunately, only certain nuclear isotopes undergo the fission process:
235U only 0.7% of naturally occurring U(99.3% is 238U, which doesn’t fission)
239Pu doesn’t occur naturally, but is produced in nuclear reactors
…. There are other fissionable isotopes, e.g. 233U &232Th, but they are very rare
Little boy (235U)
(doughnut-like)
Fat man (239Pu)
Devastation
Hiroshima Aug 6 1945 8:15AM
80,000 people killed immediately;
~100,000 people were exposed to lethal radiation & died painful slow deaths
Hiroshima aftermath
Devastation
Nagasaki Aug 9 1945 10:45AM
39,000 people killed immediately;
~70,000 people were exposed to lethal radiation & died painful slow deaths
Nagasaki aftermath
Nuclear fusion
2H + 3H 4He + n
Two light nuclei fuse togetherto form a heavier one
Here the nuclei have to start outwith large energy in order to
overcome the electrical repulsion
Energy balance in a fusion reaction
4He+n
12.3 MeV KE heat 2H +3H
Need to overcome electric repulsion
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Protons need ~2MeVenergy to get within10-15 m of each other(where strong nuclear force can be felt)
This requires super-hightemperatures (severalMillion degrees). Such hightemperatures exist in thecore of the Sun or in an Atomic-Bomb explosion
H-bomb: powered by nuclear fusion
Nuclear fission bomb “detonator”produces the high temperature
required to initiate fusion processes
Nuclear fusion bomb
Brighter than 1000 suns
1000 times the power of an A-bomb!!
Dangers of teaching nuclear physics
Oh, and I suppose it
was me who said ‘what
harm could it be to give the
chickens a book on nuclear
physics?’
Fusion in the Sun
The core temperatureis ~14 million degrees
Here a tiny fractionof the protons haveenough thermal energyto undergo fusion
Solar fusion
processes
+ 5.5 MeV
+ 1.4 MeV
+ 12.9 MeV
pp-cycle
6 protons 4He + 2 protons + 2 “positrons” + 2neutrinos
Energy balance in the pp-cycle
4He
25 MeV KE heat 4 protons
+ 2 neutrinos
How do we know what goes oninside the Sun?
Superkamiokande
Superkamiokande
Direction of neutrinosdetected in Superkamiokande
Sun as seen by a neutrino detector
Neutrinos come directly from solar core
Neutrinos are everywhere
T esttest