Binding Energy & Nuclear Stability

By the end of this workbook you should be able to:

Define binding energy and mass defect, and explain the relationship between them.
Apply Einstein's mass–energy equivalence, E = mc², to calculate binding energies and the energy released in nuclear reactions.
Interpret the binding energy per nucleon curve, and use it to explain why both fission and fusion release energy.
Explain the role of the strong nuclear force in nuclide stability, including the significance of the neutron-to-proton ratio.
Describe how the discrete alpha and gamma spectra, and the continuous beta spectrum, provide evidence for nuclear energy levels and for the neutrino.
Calculate the energy released in specific fission and fusion reactions, and explain how a chain reaction is sustained and controlled.
Describe the role of control rods, the moderator, the heat exchanger and shielding in a nuclear power plant, and explain how fission products are managed as nuclear waste.

Name

1. Binding energy and mass defect

Nucleons inside a nucleus are held together by the strong nuclear force. To pull a nucleus completely apart into its separate, stationary protons and neutrons, energy has to be supplied from outside — in exactly the same way that energy has to be supplied to separate two magnets that are stuck together. This leads to a key definition:

Binding energy: The binding energy of a nucleus is the energy that would be needed to completely separate it into individual, stationary protons and neutrons. Equivalently, it is the energy that would be released if a nucleus were assembled from separate nucleons. Binding energy is always taken to be a positive quantity — the more strongly bound (the more stable) a nucleus is, the larger its binding energy.

Fig. 1.1 — A bound nucleus has less energy than the same nucleons completely separated. The gap between the two levels is the nucleus's binding energy, whichever direction you cross it in.

Einstein's mass–energy equivalence, E = mc², tells us that any change in the energy of a system is accompanied by a change in its mass. In everyday processes the mass changes involved are far too small to detect — heating 2.0 kg of water by 5.0 °C transfers Q = mcΔT = 2.0 × 4180 × 5.0 = 4.18 × 10⁴ J into the water, corresponding to a mass increase of only Δm = E/c² ≈ 4.6 × 10⁻¹³ kg. But the energies released in nuclear reactions are millions of times larger relative to the masses involved, so the associated mass changes become measurable — and central to how binding energy is actually calculated.

Units for very small masses: Kilograms are inconveniently large for particles as small as nucleons, so nuclear physicists use the (unified) atomic mass unit, u — defined as exactly one twelfth of the mass of a carbon-12 atom.

Particle	Mass / kg	Mass / u	Mass / MeV c⁻²
electron	9.109 × 10⁻³¹	0.000549	0.511
proton	1.673 × 10⁻²⁷	1.007276	938
neutron	1.675 × 10⁻²⁷	1.008665	940

The conversion between the last two columns uses the fact that 1 u = 931.5 MeV c⁻² — the energy that would be released if 1 u of mass were entirely converted into energy.

Worked example 1.1

A helium-4 atom has a mass of 4.00260 u. It consists of 2 protons (1.007276 u each), 2 neutrons (1.008665 u each) and 2 electrons (0.000549 u each). Calculate its mass defect and binding energy.

Answer

Total mass of separated particles = 2(1.007276) + 2(1.008665) + 2(0.000549) = 4.03298 u
Mass defect Δm = 4.03298 − 4.00260 = 0.03038 u

Fast method (use 931.5 MeV/u directly): BE = 0.03038 × 931.5 = 28.3 MeV

Slow method (convert to kg and J first): Δm = 0.03038 × 1.6605×10⁻²⁷ = 5.04×10⁻²⁹ kg; E = Δmc² = 4.53×10⁻¹² J = 2.83×10⁷ eV = 28.3 MeV

Both routes must agree — the 931.5 MeV/u shortcut is simply the slow method with the unit conversions already done for you.

Worked example 1.2

Radium-226 decays by alpha emission: ²²⁶₈₈Ra → ²²²₈₆Rn + ⁴₂α. The rest masses are: Ra-226 = 226.0254 u, Rn-222 = 222.0176 u, alpha particle = 4.0026 u. Calculate the energy released.

Answer

Δm = (222.0176 + 4.0026) − 226.0254 = −0.0052 u (the products have less mass than the parent)
Energy released = 0.0052 × 931.5 = 4.8 MeV, shared as kinetic energy between the radon nucleus and the alpha particle.

Play with the simulation below: it holds real nuclide masses for a wide range of isotopes, and will show you the working for the binding energy of any nuclide you choose.

Use the Binding Energy Curve tab to explore any nuclide's binding energy per nucleon; use the Reactions tab to calculate the energy released in specific fission and fusion reactions.

An interactive simulation normally appears here — view this workbook on a device to use it.

1A helium-3 nucleus has a mass of 3.014932 u. It consists of two protons (1.007276 u each) and one neutron (1.008665 u). Calculate its mass defect and binding energy, in MeV.

total nucleon mass = 2(1.007276) + 1.008665 = 3.023217 u; mass defect = 3.023217 − 3.014932 = 0.008285 u; BE = 0.008285 × 931.5 = 7.72 MeV.

2A nuclear reaction releases 6.0 MeV of energy. Calculate the corresponding decrease in mass, in kg.

E = 6.0 MeV = 9.61 × 10⁻¹³ J; Δm = E/c² = (9.61 × 10⁻¹³)/(9.00 × 10¹⁶) ≈ 1.07 × 10⁻²⁹ kg.

3Explain why binding energy is always quoted as a positive quantity, even though it corresponds to a negative nuclear potential energy.

binding energy is defined as the energy that would need to be supplied to separate the nucleus (the opposite sign to the nuclear potential energy itself), so that a larger, positive binding energy corresponds intuitively to a more stable, more tightly-bound nucleus.

2. Binding energy per nucleon, fission & fusion

Bigger nuclei naturally have more total binding energy, simply because they contain more nucleons — so total binding energy on its own is not a fair way to compare how stable different nuclides are. Instead, physicists divide by the number of nucleons:

Binding energy per nucleon: binding energy per nucleon = (total binding energy) / (number of nucleons, A). This is a much better guide to a nucleus's stability: the larger the binding energy per nucleon, the more tightly bound — and more stable — the nucleus is.

Fig. 2.1 — The binding energy per nucleon curve, plotted from measured nuclide mass data across the periodic table (nucleon number A against binding energy per nucleon; iron-56 and other points from the class dataset, nickel-62 added from AME nuclide mass tables since it fell outside the class dataset's sample). The curve peaks at nickel-62 (8.79 MeV/nucleon), narrowly ahead of iron-56 — both fusion of light nuclei and fission of heavy nuclei move the products towards this peak, releasing energy.

Two features of this curve matter enormously:

The curve rises steeply for the lightest nuclides, reaches a broad maximum around iron-56 and nickel-62 (binding energy per nucleon ≈ 8.8 MeV), and then declines slowly for heavier nuclides.
Above about A = 60, the curve is almost flat — adding more nucleons keeps increasing the total binding energy, but barely changes the binding energy per nucleon (Section 3 explains why, in terms of the strong force's short range).

Fission and fusion, in terms of the curve: Nuclear fission is the splitting of a massive nucleus into two smaller nuclei. Because the fragments sit further up (further left along) the curve than the original heavy nucleus, they are more tightly bound — the reaction releases energy.

Nuclear fusion is the combination of two very light nuclei into a single, more massive nucleus. Because the new nucleus sits further up (further right along) the curve than the original light nuclei, it is more tightly bound — the reaction also releases energy.

Either way, the products end up with less total mass than the reactants — the "missing" mass has been converted directly into the kinetic energy of the products, via E = mc². Both fission and fusion are just two different routes towards the same destination: the peak of the binding-energy-per-nucleon curve.

Worked example 2.1

Iron-56 has a binding energy per nucleon of about 8.8 MeV. Estimate the total binding energy of one mole of iron-56 nuclei, in joules.

Answer

Total binding energy per nucleus = 56 × 8.8 = 493 MeV = 493 × 10⁶ × 1.60 × 10⁻¹⁹ J = 7.89 × 10⁻¹¹ J
For one mole (6.02 × 10²³ nuclei): total ≈ (7.89 × 10⁻¹¹) × (6.02 × 10²³) = 4.75 × 10¹³ J — for comparison, a similar mass of coal releases roughly a million times less energy when burned.

Switch to the Reactions tab in the simulation above to see this play out for specific fission and fusion reactions — choose a reaction from the dropdown, and the tool will show you the binding energy per nucleon of every nuclide involved and let you calculate the energy released.

4Use a binding energy per nucleon of about 8.8 MeV for nickel-62 to estimate its total binding energy, in MeV.

62 × 8.8 ≈ 546 MeV.

5A uranium-238 nucleus (binding energy per nucleon ≈ 7.6 MeV) fissions into two nuclei each of nucleon number 119 (binding energy per nucleon ≈ 8.5 MeV). Estimate the energy released, in MeV.

BE before = 238 × 7.6 = 1808.8 MeV; BE after = 2 × (119 × 8.5) = 2023 MeV; energy released ≈ 2023 − 1808.8 ≈ 214 MeV.

6Explain, in terms of the binding energy curve, why fusing two nuclei that are already close to iron-56 would not release energy.

iron-56 already sits at (or essentially at) the peak of the curve, so fusing two nuclei from around there would produce a product with a similar or lower binding energy per nucleon — no energy is released (and energy may even need to be supplied).

3. The strong nuclear force and nuclide stability

Inside a nucleus, every pair of protons repels every other proton electrically — yet nuclei with many protons packed closely together clearly do not fly apart. Some other, stronger, attractive force must be at work between nucleons. In 1935 the Japanese physicist Hideki Yukawa proposed that nucleons attract each other by constantly exchanging short-lived particles (later called mesons) — his hypothesis was strongly supported when mesons were actually discovered experimentally in 1947, providing direct evidence that the strong nuclear force is real.

Fig. 3.1 — In a stable nucleus, the short-range attractive strong nuclear force between neighbouring nucleons balances the longer-range repulsive Coulomb force between protons.

Why heavier stable nuclides need proportionally more neutrons: Because the strong force has a very short range, each nucleon really only "feels" its nearest neighbours. The Coulomb repulsion between protons, by contrast, has an unlimited range — every proton repels every other proton in the nucleus, however far apart they are. As nuclei get larger, this accumulating repulsion becomes more significant relative to the strictly local strong-force attraction. Adding extra neutrons increases the attractive strong force without adding any extra repulsion, which is why heavier stable nuclides need progressively more neutrons per proton than lighter ones.

Fig. 3.2 — The line (belt) of stability, drawn to the actual proton and neutron numbers of real nuclides (compare with a data booklet chart of the nuclides). Stable nuclides (gold line) lie close to N = Z for small Z but drift to progressively larger N/Z ratios for heavier elements, sitting inside a wider band of unstable isotopes that thins out at both the neutron-rich and proton-rich edges. No stable nuclides exist above lead-208 (Z = 82, N = 126).

Recall from Section 2 that the binding energy curve is almost flat above A ≈ 60. This follows from the same short-range argument: once a nucleus is big enough that a typical nucleon's nearest neighbours no longer change much as more nucleons are added further away, each additional nucleon contributes roughly the same amount to the total binding energy — but does very little to change the average (per-nucleon) value, since it's mostly interacting with the same limited set of close neighbours that any other nucleon does.

7Silver-107 (Z = 47) is a stable nuclide. Calculate its N/Z ratio.

N = 107 − 47 = 60; N/Z = 60/47 ≈ 1.28.

8Suggest why no stable nuclides exist with a proton number greater than 82 (lead).

beyond lead-208, the accumulated long-range Coulomb repulsion between the large number of protons always outweighs the short-range strong-force attraction available, however many extra neutrons are added, so no arrangement of nucleons is stable.

9Explain why the binding energy per nucleon changes very little as nucleons are added to a nucleus that already has more than about 60 nucleons.

each nucleon only strongly interacts with its close neighbours (short-range strong force); once a nucleus is bigger than about 60 nucleons, adding another nucleon still adds roughly the same fixed contribution to the total binding energy, so the average (per-nucleon) value barely changes.

4. Nuclear energy levels: evidence from spectra

Just as atomic electrons occupy only certain discrete energy levels, nuclei themselves have discrete internal energy levels. The evidence comes from carefully measuring the energies of the radiation nuclei emit.

Alpha and gamma spectra: discrete energies. Americium-241 decays by alpha emission to neptunium-237. Almost all of the alpha particles emitted are found to have one single, precise energy — but a small fraction are emitted with one of a few other, slightly lower, precise energies. Each of these corresponds to the neptunium-237 nucleus being left in a different discrete excited state, which then very quickly loses its extra energy by emitting a gamma-ray photon of correspondingly discrete energy as it drops down to its ground state (or to another, lower excited state).

Fig. 4.1 — Alpha particles of different (but discrete) energies leave the daughter nucleus in different discrete excited states; each excited state then decays to a lower level by emitting a gamma-ray photon of discrete energy. Both spectra are evidence for discrete nuclear energy levels.

Historical note

Beta particles behave completely differently: particles emitted from the same radionuclide come out with a continuous range of energies, from zero up to some maximum, rather than one or a few discrete values. At first this seemed to threaten conservation of energy and momentum themselves — if a nucleus simply emitted one electron, simple two-body decay would force every electron to have exactly the same energy, just as every alpha particle from a given decay does. In 1930 the Austrian physicist Wolfgang Pauli proposed a bold solution: a third, almost undetectable particle — later named the neutrino (or antineutrino, for beta-minus decay) — is emitted alongside the electron in every beta decay. Sharing the released energy between three particles rather than two allows the electron's individual energy to vary continuously, depending on the angles at which the three products happen to fly apart, while the total energy and momentum released stay exactly conserved. Neutrinos were not actually detected until 1956 — 26 years after Pauli's proposal — because they interact so weakly with matter that trillions pass through every square centimetre of the Earth every second without being stopped.

Fig. 4.2 — The beta particle energy spectrum is continuous, unlike the discrete spectra of alpha particles and gamma rays — the key clue that led to the discovery of the neutrino.

10Explain how the existence of several discrete alpha particle energies from a single radionuclide provides evidence for discrete energy levels within the daughter nucleus.

each discrete alpha energy corresponds to the daughter nucleus being left in one particular internal state; since only a few, discrete alpha energies are ever observed (not a continuous range), the daughter nucleus must only be able to exist in a few discrete internal energy states.

11Explain why the continuous energy spectrum of beta particles was, historically, a serious puzzle for physicists.

a two-body decay (nucleus → daughter + electron only) would force every emitted electron to have exactly the same, single energy, by conservation of energy and momentum — yet a continuous range was observed, apparently threatening conservation of energy itself.

12State the role played by the neutrino (or antineutrino) in resolving this puzzle, and suggest why neutrinos are so difficult to detect.

a third particle (the neutrino/antineutrino) shares the released energy and momentum with the electron, allowing the electron's own energy to vary continuously depending on the relative directions of the three products; neutrinos are hard to detect because they have no charge and interact only via the weak force, so they pass through enormous amounts of matter without interacting.

5. Fission and fusion in practice

Binding energy is not just an abstract curve — it is the physics behind how a large share of the world's electricity is generated, and behind the process that powers every star, including our own Sun. This section applies the ideas from Sections 1–3 to real fission and fusion reactions: how much energy a single reaction releases, how a chain reaction can be sustained and controlled, how a nuclear power plant is engineered around that chain reaction, and what happens to the radioactive fission products it leaves behind.

Energy released in fission and fusion

Spontaneous fission: some very heavy nuclides (such as uranium-238 or californium-252) occasionally split apart entirely on their own, with no external trigger — one further mode of radioactive decay available to the heaviest nuclides, alongside alpha and beta decay.

Induced fission: a nucleus (such as uranium-235) is made to split by capturing a slow-moving ("thermal") neutron, forming a highly unstable compound nucleus that immediately splits into two fission fragments plus further neutrons. This is the process harnessed in nuclear reactors, since each reaction releases more neutrons that can go on to trigger further fissions.

13State one similarity and one difference between spontaneous fission and induced fission.

Similarity: both are ways a massive nucleus splits into two smaller, more tightly-bound fragments, releasing energy. Difference: spontaneous fission happens on its own, entirely at random, like any other mode of radioactive decay; induced fission only happens once a nucleus captures an incoming neutron.

Worked example 5.1 — energy from a single fission

A slow-moving neutron is captured by a uranium-235 nucleus, which undergoes induced fission to produce barium-144 and krypton-89, releasing further neutrons.

(a) Write a balanced nuclear equation for this reaction.
(b) Using the rest masses below, calculate the energy released, in MeV.

Rest mass of ¹₀n = 1.0087 u · ²³⁵₉₂U = 235.0439 u · ¹⁴⁴₅₆Ba = 143.9229 u · ⁸⁹₃₆Kr = 88.9178 u · 1 u = 931.5 MeV/c²

Answer

(a) ¹₀n + ²³⁵₉₂U → ¹⁴⁴₅₆Ba + ⁸⁹₃₆Kr + 3 ¹₀n
(check: mass numbers 1 + 235 = 236 = 144 + 89 + 3; protons 92 = 56 + 36 ✓)

(b) mass before = 1.0087 + 235.0439 = 236.0526 u
mass after = 143.9229 + 88.9178 + 3(1.0087) = 235.8668 u
Δm = 236.0526 − 235.8668 = 0.1858 u
E = 0.1858 × 931.5 ≈ 173 MeV

Worked example 5.2 — energy from a single fusion

A deuterium (²₁H) nucleus fuses with a tritium (³₁H) nucleus to form helium-4 and a neutron — the reaction targeted by experimental fusion reactors such as ITER.

(a) Write the equation for this reaction.
(b) Using the rest masses below, calculate the energy released, in MeV.

²₁H = 2.014102 u · ³₁H = 3.016049 u · ⁴₂He = 4.002602 u · ¹₀n = 1.008665 u

Answer

(a) ²₁H + ³₁H → ⁴₂He + ¹₀n

(b) mass before = 2.014102 + 3.016049 = 5.030151 u
mass after = 4.002602 + 1.008665 = 5.011267 u
Δm = 5.030151 − 5.011267 = 0.018884 u
E = 0.018884 × 931.5 ≈ 17.6 MeV

Try it yourself: adjust the temperature and confinement pressure below to see the conditions needed to force two nuclei together in fusion, and compare with the conditions needed to trigger fission.

Increase the temperature and confinement pressure sliders to see the conditions needed to force nuclei together in fusion, then switch to the Nuclear Fission tab to compare.

An interactive simulation normally appears here — view this workbook on a device to use it.

If the simulation does not load above, open it directly in a new tab ↗.

Interactive simulation by Dr Jones Physics — drjonesphysics.com/fusion-fission-2. Used with permission.

14Plutonium-239 absorbs a slow neutron and undergoes induced fission, producing xenon-134 and zirconium-103 plus further neutrons. (a) Balance the nuclear equation. (b) Using the rest masses ¹₀n = 1.00867 u, ²³⁹₉₄Pu = 239.0521634 u, ¹³⁴₅₄Xe = 133.9053945 u and ¹⁰³₄₀Zr = 102.92660 u, calculate the energy released, in MeV.

(a) ¹₀n + ²³⁹₉₄Pu → ¹³⁴₅₄Xe + ¹⁰³₄₀Zr + 3 ¹₀n (mass numbers: 1 + 239 = 240 = 134 + 103 + 3; protons: 94 = 54 + 40 ✓). (b) mass before = 1.00867 + 239.0521634 = 240.0608334 u; mass after = 133.9053945 + 102.92660 + 3(1.00867) = 239.8580045 u; Δm = 0.2028 u; E = 0.2028 × 931.5 ≈ 189 MeV.

15The Sun is powered by the proton–proton chain, whose overall effect is the fusion of four hydrogen-1 nuclei into one helium-4 nucleus (releasing two positrons and two neutrinos along the way). Using the atomic masses ¹₁H = 1.007825 u and ⁴₂He = 4.002602 u, estimate the total energy released per helium-4 nucleus formed.

Δm = 4(1.007825) − 4.002602 = 4.031300 − 4.002602 = 0.028698 u; E = 0.028698 × 931.5 ≈ 26.7 MeV. (In reality a small fraction of this escapes the Sun immediately as the kinetic energy of the two neutrinos, which interact so weakly that they barely notice the rest of the star on their way out — see Section 4.)

Chain reactions

Chain reaction: each induced fission of a U-235 nucleus releases on average two or three new neutrons. If, on average, at least one of these neutrons goes on to cause a further fission, the reaction becomes self-sustaining — a chain reaction. Physicists describe the state of the reaction using the number of fissions each fission goes on to cause, on average:

Subcritical — fewer than one further fission per fission, on average: the reaction dies away.
Critical — exactly one further fission per fission, on average: the fission rate (and power output) stays constant. This is how a working reactor is operated.
Supercritical — more than one further fission per fission, on average: the fission rate grows, either briefly and under control (to raise a reactor's power output) or uncontrolled (as in a weapon).

Try it yourself: choose a number of uranium-235 nuclei, populate the grid, then insert some neutrons and watch whether the chain reaction dies out, ticks over steadily, or runs away — and see how the result depends on how densely packed the uranium-235 nuclei are.

Choose a number of uranium-235 nuclei, populate the grid, then insert neutrons and watch the chain reaction spread.

An interactive simulation normally appears here — view this workbook on a device to use it.

Interactive simulation by Dr Jones Physics — drjonesphysics.com/chain. Used with permission.

16Use the terms subcritical, critical and supercritical to explain how a nuclear power station keeps its fission chain reaction running at a constant, controllable rate rather than letting it grow uncontrollably.

A working reactor is operated critical: on average exactly one neutron from each fission goes on to cause another fission, so the fission rate — and therefore the power output — stays constant. If the reaction starts to become supercritical, more neutrons are causing new fissions than are being lost, so control rods are inserted further to absorb the excess neutrons and return the reactor to critical; if it becomes subcritical, fewer neutrons cause new fissions than are lost, and the reaction dies away.

Stretch: why light nuclei make the best moderators

The neutrons released by fission travel at roughly 10⁷ m s⁻¹ — far too fast to be efficiently captured by U-235 nuclei, which react best with much slower ("thermal") neutrons. A moderator slows fast neutrons down through repeated elastic collisions with the nuclei of the moderator material. Think of a game of snooker: a moving ball transfers the largest share of its kinetic energy to a stationary ball of similar mass in a head-on collision, but bounces off a much heavier ball having lost almost none of its energy. Since a neutron has almost exactly the same mass as a hydrogen nucleus, water (or "heavy water", containing deuterium) is an extremely effective moderator — each collision can remove a large fraction of a neutron's kinetic energy. Graphite (carbon-12 nuclei, about 12 times a neutron's mass) is a less efficient but still workable alternative, requiring more collisions to achieve the same slowing.

Inside a nuclear power plant

A nuclear power plant is built around the fission chain reaction: it needs a way to control the reaction's rate, a way to sustain it efficiently, a way to move the released energy out to generate electricity, and a way to keep everyone outside safe. Label the diagram below, then read on to see how each part does its job.

Drag each label below onto the correct part of the nuclear power plant diagram (or click a label, then click a target box). The other parts are labelled for you.

Reactor pressure vessel

Fuel rods

Coolant pump

Steam to turbines

Water from turbines

Drop label here

Moderator

Shielding / containment

Control rods

Heat exchanger

Control rods are made of a strongly neutron-absorbing material, such as boron or cadmium. Raising or lowering them into the reactor core changes how many of the neutrons released by fission are absorbed rather than going on to cause further fissions, which is how the reaction's rate — and so the plant's power output — is adjusted, or the reactor shut down entirely in an emergency.

The moderator (often the water that also acts as the primary coolant) slows fast fission neutrons down to thermal speeds through the elastic collisions described above, making them far more likely to cause a further U-235 fission and sustain the chain reaction efficiently.

The heat exchanger transfers heat from the primary coolant loop, which has been in direct contact with the radioactive reactor core, to a completely separate secondary loop that carries the resulting steam to the turbines. Keeping the two loops physically separate means the water driving the turbines (and everything downstream of it) never becomes radioactively contaminated.

Shielding — a thick structure of concrete, steel and other dense materials surrounding the reactor — absorbs radiation (particularly neutrons and gamma rays) escaping from the core, protecting workers and the public, and also helps contain radioactive material in the event of an accident.

17Explain why a nuclear reactor's coolant is kept in a separate primary loop, rather than the same water being sent directly to drive the turbines.

The primary coolant is in direct contact with the reactor core and becomes radioactively contaminated; keeping it in a closed loop, and transferring its heat to a separate secondary loop via a heat exchanger, means the steam sent to the turbines (and the turbine hall itself) stays free of radioactive contamination.

18A reactor operator wants to reduce the plant's power output. Explain what they should do to the control rods, and why this works.

They should lower (insert further) the control rods. This increases the amount of neutron-absorbing material within the core, so a smaller fraction of the neutrons released by fission go on to cause further fissions; the reaction becomes closer to subcritical, so the fission rate — and the power output — falls.

What happens to the fission products?

The fission fragments produced by a reaction — barium-144 and krypton-89 in Worked example 5.1, for instance — are themselves radioactive. Heavy nuclides need a higher neutron-to-proton ratio than lighter nuclides to be stable (Section 3), so fission fragments inherit a neutron-to-proton ratio that is far too high for their new, smaller mass number. They are almost always neutron-rich and unstable, decaying by beta-minus emission — often followed by gamma emission, and sometimes through several successive decays — before finally reaching a stable nuclide. Their half-lives vary enormously, from fractions of a second to hundreds of thousands of years, so nuclear waste is not a single hazard but a mixture that has to be managed differently depending on how active, and how long-lived, each component is.

Classifying nuclear waste:

High-level waste — spent fuel and the most intensely radioactive fission products: small in volume, but very hot and highly radioactive.
Intermediate-level waste — reactor components and other material with significant but lower activity, produced in larger volumes.
Low-level waste — protective clothing, tools and other lightly contaminated material: low activity, but the largest volume by far.

Spent fuel is first stored underwater in cooling ponds at the reactor site for several years — the water shields the surrounding area from radiation and carries away the heat the fuel continues to generate — before being moved to sealed dry cask storage. For permanent disposal, high-level waste can be vitrified: fused with glass-forming materials into solid glass blocks, sealed inside steel canisters, and buried deep underground in stable geological rock formations, isolating it for the tens of thousands of years its activity takes to fall to safe levels. Some countries instead reprocess spent fuel, chemically separating out the unused uranium and plutonium so it can be reused as new fuel, which reduces the volume of waste that needs long-term storage.

19Explain why the fission fragments produced in a reactor are radioactive, and describe one method used for the long-term management of high-level nuclear waste.

Fission fragments inherit the high neutron-to-proton ratio of the heavy nuclide they came from, but the stable nuclides of their (much smaller) mass number need a lower neutron-to-proton ratio — so fission fragments are neutron-rich and unstable, decaying by beta-minus (often followed by gamma) emission, sometimes through several stages, until they reach a stable nuclide. One management method: liquid high-level waste is vitrified into solid glass blocks, sealed in steel canisters, and buried deep underground in a stable geological rock formation, isolating it until its activity has fallen to safe levels.

Glossary

Binding energy: The energy that would be needed to completely separate a nucleus into individual, stationary protons and neutrons; equivalently, the energy released if the nucleus were assembled from separate nucleons.
Mass defect: The difference between the total mass of a nucleus's separate, individual nucleons and the actual (smaller) mass of the assembled nucleus.
Mass–energy equivalence: Einstein's relationship E = mc², which states that any change in the energy of a system corresponds to a proportional change in its mass.
Unified atomic mass unit, u: A unit of mass defined as exactly one twelfth of the mass of a carbon-12 atom, convenient for expressing the masses of nucleons and nuclides.
Nucleon: A collective term for the particles found in the nucleus — protons and neutrons.
Binding energy per nucleon: The total binding energy of a nucleus divided by its nucleon number, A; the best single measure of how tightly bound (stable) a nuclide is.
Fission: The splitting of a massive nucleus into two smaller, more tightly bound nuclei, releasing energy.
Fusion: The combination of two very light nuclei into a single, more massive, more tightly bound nucleus, releasing energy.
Strong nuclear force: The short-range attractive force between nucleons that holds the nucleus together, overcoming the electrostatic repulsion between protons.
Line (belt) of stability: The narrow band of neutron-to-proton ratios, plotted on a graph of N against Z, within which stable nuclides are found.
Chain reaction: A self-sustaining sequence of fission reactions, in which the neutrons released by each fission go on to trigger further fissions.
Critical (of a chain reaction): The state in which, on average, exactly one neutron from each fission goes on to cause a further fission, keeping the fission rate constant — the normal operating state of a nuclear reactor.
Moderator: A material (such as water or graphite) that slows fast fission neutrons to thermal speeds through elastic collisions, making them far more likely to cause further fission.
Control rods: Neutron-absorbing rods (e.g. boron or cadmium) raised or lowered within a reactor core to regulate, or shut down, the fission chain reaction.
Heat exchanger: A device that transfers heat from a reactor's (radioactive) primary coolant loop to a separate secondary loop, without the two fluids mixing.
High-level waste: Spent nuclear fuel and the most intensely radioactive fission products; small in volume but very hot and highly radioactive.