Nuclear Fusion

Branch note: This page deepens one part of Nuclear Physics.

Overview

Nuclear Fusion is the joining of light nuclei to form a heavier nucleus. It powers stars and is studied as a possible future energy source on Earth.

The essential H2 Physics idea is:

light nuclei combine -> products have greater total binding energy -> total rest mass decreases -> energy is released

Fusion is not simply “nuclei join, so energy appears”. The energy comes from a decrease in total rest mass and an increase in total binding energy. Binding energy per nucleon shows the relevant curve trend, but a reaction calculation must compare total binding energies.

Syllabus scope note: The H2 Physics syllabus focuses on the physics of nuclear fusion, including conservation laws, mass defect, binding energy, and binding energy per nucleon. Plasma, confinement methods, fusion reactors, and controlled-fusion engineering are included here as useful background for conceptual understanding, but they are not explicitly required by the syllabus.

This topic links closely with:

• Nuclear Physics
• Nuclear Fission
• Ionizing Radiation and Safety

Core Ideas

• Fusion combines light nuclei to form a heavier nucleus.
• The products can have greater binding energy per nucleon than the reactants.
• The total rest mass after the reaction is lower than before the reaction.
• The released energy is given by $E=\Delta m{c}^2$.
• Positively charged nuclei repel each other, so very high temperatures help suitable nuclei approach closely enough to fuse.

Context / enrichment ideas:

• At fusion temperatures, the fuel exists as a plasma.
• Useful controlled fusion requires sufficient heating, density, and confinement at the same time.

What Is Fusion?

Fusion occurs when two light nuclei come close enough for the short-range strong nuclear force to bind them into a heavier nucleus.

Two competing interactions are important:

• electrostatic repulsion between positively charged nuclei acts over a relatively long range
• the strong nuclear force is attractive but acts only over a very short range

Before fusion can occur, the nuclei must come close enough for the strong nuclear force to dominate.

Fusion differs from fission:

Process	Basic Change	Typical Region	Energy Reason
Fusion	Light nuclei combine	Low nucleon number	Products can have greater total binding energy
Fission	Heavy nucleus splits	High nucleon number	Products can have greater total binding energy

Representative Context: Deuterium-Tritium Fusion

Representative rather than required reaction recall

The D–T equation is the worked example used in this wiki to practise conservation and energy accounting. The explicit Topic 20 outcome is the relevance of binding energy per nucleon to fusion; recalling this particular reaction is not an additional syllabus requirement.

A common fusion reaction is:

$${}_1^2\mathrm{H}+{}_1^3\mathrm{H}\to {}_2^4\mathrm{He}+{}_0^1\mathrm{n}+E$$

where:

• ${}_1^2\mathrm{H}$ is deuterium
• ${}_1^3\mathrm{H}$ is tritium
• ${}_2^4\mathrm{He}$ is a helium-4 nucleus
• ${}_0^1\mathrm{n}$ is a neutron
• $E$ is the released energy

Figure: Deuterium and tritium fuse to form helium-4, a neutron, and released energy, while conserving nucleon number and proton number.

Conservation checks:

Quantity	Reactants	Products	Conserved?
Nucleon number	$2+3=5$	$4+1=5$	Yes
Proton number / charge	$1+1=2$	$2+0=2$	Yes

The neutron is not a side detail: it is one of the products and can carry substantial kinetic energy. It also creates engineering and shielding issues in real reactors.

Why Energy Is Released

Mass Defect Explanation

For the D–T reaction, the total rest mass of the products is less than the total rest mass of the reactants:

$$\Delta m=m_{\text{reactants}}-m_{\text{products}}$$

The decrease in total rest energy corresponds to the released energy:

$$E=\Delta m{c}^2$$

Using the source-note values:

$$\Delta m=2.0141+3.0161-(4.0026+1.0087)=0.0189\mathrm{u}$$

This corresponds to about:

$$17.6\mathrm{MeV}$$

When atomic masses are used for this reaction, the electron masses cancel: the deuterium and tritium atoms contain two electrons in total, and the helium atom also contains two electrons.

Binding Energy Explanation

Binding energy is the energy needed to separate a nucleus completely into its nucleons.

Binding energy per nucleon tells us how tightly bound the average nucleon is. A greater value means greater average binding, but it is not by itself a universal predictor of half-life or every possible decay mode.

For fusion of light nuclei:

• reactants are light nuclei with relatively low binding energy per nucleon
• the product nucleus is more tightly bound
• total binding energy increases
• the increase in binding energy is released as energy

So the same energy release can be calculated as:

$$E=\text{total B.E. of products}-\text{total B.E. of reactants}$$

The source note evaluates the D–T reaction using binding energies and obtains about:

$$17.7\mathrm{MeV}$$

The small difference from the mass calculation is due to rounding.

Binding Energy Per Nucleon And Fusion

The binding-energy-per-nucleon curve rises steeply for light nuclei and reaches a broad maximum in the iron–nickel region, near $A\approx 56$ to $62$.

For this fusion branch, the key part is the left side of the curve:

• light nuclei can fuse into a heavier product
• the product is closer to the high-binding-energy region
• the product is more tightly bound
• energy is released

Figure: Fusion of suitable light nuclei can form a product nearer the high-binding-energy region. Energy is released only when the product has greater total binding energy than the reactants, equivalently a smaller total rest mass; the graph’s vertical axis is binding energy per nucleon, so nucleon numbers must still be included in a calculation.

Keep the reasoning precise:

Fusion releases energy when the final products have greater total binding energy than the initial nuclei.

This figure is qualitative. It shows why suitable light nuclei can release energy by fusion; it is not a precise graph for reading numerical binding energies.

Why Very High Temperature Is Needed

The need for very high temperature is part of the core qualitative fusion model. Detailed plasma behaviour and confinement engineering are enrichment, but students should understand why ordinary thermal energies are not enough.

Nuclei are positively charged, so they repel each other through the Coulomb force.

For fusion to occur, nuclei must approach closely enough for the strong nuclear force to act. This requires some collisions to have very high kinetic energy.

Temperature is related to the average kinetic energy of particles. Therefore, very high temperature helps because nuclei move faster on average.

Figure: Positive nuclei repel each other, so very high temperature is needed for some collisions to bring nuclei close enough for fusion.

The source note includes a discussion question referring to deuterium fusion temperatures of order:

$$1.0\times 10^7\mathrm{K}$$

The exact value is less important here than the qualitative point:

very high temperature -> high kinetic energy -> better chance of close nuclear encounters

However, high temperature alone is not enough. The fuel must also remain dense and confined long enough.

Enrichment: Controlled Fusion Context — Plasma

Plasma is included to provide context for controlled fusion. Detailed plasma behaviour is beyond the explicit H2 Physics syllabus.

At fusion temperatures, atoms are ionised. The fuel becomes plasma, containing:

• positive ions
• free electrons

Plasma is not an ordinary hot gas in a container. It is electrically conducting, responds to magnetic fields, and would damage ordinary material walls if it touched them at fusion temperatures.

Enrichment: Controlled Fusion Context — Confinement

Controlled fusion requires plasma confinement. The different confinement methods are included here as enrichment rather than explicit syllabus content.

Confinement means keeping the hot fusion fuel together long enough for useful fusion reactions to occur.

Fusion fuel must satisfy three linked requirements:

• high temperature
• sufficient density
• sufficient confinement time

If the plasma escapes or cools too quickly, too few reactions occur and the system does not produce useful net energy.

Figure: Gravitational, magnetic, and inertial confinement all aim to keep hot fusion fuel dense enough for long enough.

For a fuller discussion of the confinement problem and why heating alone is not enough, see Fusion Conditions and Confinement.

Enrichment: Gravitational Confinement

Stars use gravity.

Their enormous mass compresses material toward the core, giving:

• very high pressure
• high density
• sustained high temperature

This is why stars can sustain fusion over long timescales.

Enrichment: Magnetic Confinement

On Earth, one approach is to use magnetic fields to guide and confine charged plasma.

Examples include:

• tokamaks
• stellarators

The aim is to keep the plasma away from reactor walls while maintaining suitable temperature and density.

Enrichment: Inertial Confinement

Another approach is to compress a small fuel pellet very rapidly using intense energy beams such as lasers.

The compression produces:

• very high density
• high temperature
• a very short fusion burst

The difficulty is that compression must be extremely symmetric and precisely timed.

Enrichment: Fusion in Stars

This section provides useful stellar context. Detailed stellar fusion processes are included as background knowledge rather than explicit H2 syllabus content.

Stars are powered by fusion in their cores.

The Sun mainly converts hydrogen into helium through a sequence of reactions. In school-level treatment, the important point is not the full stellar reaction chain, but that nuclear fusion releases energy on a scale that chemical burning cannot explain.

Gravity provides the confinement and compression needed for stellar fusion.

Enrichment: Fusion Reactors

This section provides real-world context for controlled fusion. Detailed reactor engineering and plasma confinement are beyond the explicit H2 syllabus.

A controlled fusion reactor aims to reproduce useful fusion on Earth.

The simplified sequence is:

1. heat fusion fuel until it becomes plasma
2. confine the plasma
3. allow fusion reactions to occur
4. transfer released energy to a working fluid or blanket
5. generate electricity

The main challenge is achieving reliable net energy gain while maintaining stable confinement and handling energetic neutrons.

Enrichment: Advantages of Fusion

Fusion is attractive because it can offer:

• very high energy output per mass of fuel
• fuel sources such as deuterium that are relatively abundant
• no carbon dioxide emission during operation
• no fission-type runaway neutron chain reaction
• generally less long-lived high-level waste than many fission systems

Enrichment: Challenges of Fusion

Fusion is difficult because:

• extremely high temperature is required
• plasma confinement is technically hard
• plasma can become unstable
• energy losses may exceed energy produced
• high-energy neutrons can damage materials
• commercial-scale net energy production remains a major engineering challenge

Enrichment: Safety and Waste Comparison

Fusion generally does not rely on the same self-sustaining neutron chain reaction as fission reactors. If the necessary temperature and confinement conditions fail, fusion stops.

However, fusion is not radiation-free. It can involve:

• energetic neutrons
• gamma radiation in some reactions
• activation of nearby materials
• shielding and remote-handling requirements

See Ionizing Radiation and Safety.

Short Worked Examples

Example 1: Why High Temperature Is Needed

Positively charged nuclei repel each other. Very high temperatures give nuclei high kinetic energy, so some collisions bring nuclei close enough for the short-range strong nuclear force to bind them.

Example 2: Why Energy Is Released

The products are more tightly bound than the reactants. Their total rest mass is lower, and the corresponding decrease in total rest energy is the released energy according to:

$$E=\Delta m{c}^2$$

Enrichment Example 3: Why Stars Sustain Fusion

Gravity compresses stellar material and maintains high pressure, density, and temperature in the core.

Enrichment Example 4: Why A Fusion Reactor Is Difficult

A reactor must heat fuel into plasma and confine it long enough at sufficient density. Heating alone is not enough if the plasma escapes or cools too quickly.

Exam Relevance

Core H2 Physics

• interpret and balance a supplied representative fusion equation using conservation of nucleon number and charge
• explain energy release using the rest-mass difference
• explain energy release using binding energy
• relate fusion to the binding-energy-per-nucleon curve
• explain qualitatively why very high temperature is needed for fusion

Useful Context

• recognise the D–T equation as the representative worked example used in this wiki
• recognise that controlled fusion requires plasma
• understand qualitatively that confinement is needed
• recognise that stars use gravitational confinement
• recognise that magnetic and inertial confinement are real-world approaches to controlled fusion

Detailed comparison of confinement methods is enrichment rather than an explicit H2 syllabus requirement.

Formula / Relationship Summary

Mass-Energy

$$E=\Delta m{c}^2$$

Representative D–T Fusion Example

$${}_1^2\mathrm{H}+{}_1^3\mathrm{H}\to {}_2^4\mathrm{He}+{}_0^1\mathrm{n}+E$$

Energy From Binding Energy

$$E=\text{total B.E. of products}-\text{total B.E. of reactants}$$

Stability Idea

Light nuclei can release energy by moving toward a region of greater binding energy per nucleon after fusion.

Common Exam Traps Overview

Students often confuse:

• fusion with fission
• energy released simply because nuclei join
• mass defect with “mass disappearing” rather than mass-energy conversion
• high temperature being sufficient without confinement
• stars burning chemically
• fusion producing no radiation
• fission reactor components applying directly to fusion

See Nuclear Fusion Common Exam Traps.

Quick Revision Summary

Core H2 Ideas

• fusion joins light nuclei
• conservation of nucleon number and charge applies
• energy is released because total binding energy increases
• total rest mass decreases according to $E=\Delta m{c}^2$
• very high temperature is needed because positive nuclei repel before they get close enough for the strong nuclear force to act

Context / Enrichment

• the D–T reaction is a useful representative worked example
• fusion fuel becomes plasma
• controlled fusion requires confinement
• stars use gravity for confinement
• reactors may use magnetic or inertial confinement
• controlled fusion remains technologically challenging

Links

• Nuclear Physics
• Nuclear Fission
• Mass Defect and Binding Energy
• Fusion Conditions and Confinement
• Ionizing Radiation and Safety
• Nuclear Fusion Common Exam Traps