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Fusion

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Fast Facts About
Fusion

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Principal Energy Use: Electricity
Form of Energy: Nuclear

Fusion reactions power the Sun and the stars. Fusion occurs when nuclei from two or more atoms are forced together (overcoming the Coulomb barrier*) and fuse to form a single larger nucleus. The mass of the larger nucleus is slightly less than the combined mass of the original nuclei. The lost mass is converted to energy following Einstein’s equation E = mc2, yielding A LOT of energy. 

Illustration showing deuterium and tritium nuclei fusing to create a helium nucleus and a neutron, releasing lots of energy.

Fusion offers the possibility of an abundant carbon-free energy resource with no long-lived radioactive waste. However, fusion energy is still in the research phase because we have not yet been able to make continuous and sustainable fusion reactions happen on Earth. Making fusion happen on Earth is extremely challenging (think about putting the Sun in a box).

Three broad steps are necessary for commercially viable fusion energy:

  1. Make fusion happen on Earth (we’ve done this)
  2. Get more energy out than we put in (we’ve made significant progress)
  3. Achieve continuous and sustainable fusion to generate electricity in a thermal power plant (we haven’t done this)

The world spends billions of dollars every year on research to create commercially viable fusion energy, and progress is accelerating. Global investment in private fusion companies in the twelve months leading up to July 2025 was over $2.6 billion dollars, representing more than a quarter of the total private fusion investment to date, and the number of private fusion companies has more than doubled since 2021.

*The Coulomb barrier arises because the nuclei in a plasma are all positively charged and naturally repel each other. For fusion to occur, nuclei must have sufficient kinetic energy to overcome this electrostatic repulsion and get close enough to fuse.


Fusion Fuels (Hydrogen Isotopes)

Deuterium

  • Abundant resource (33 mg of deuterium in every m3 of seawater, which could power over 300,000 U.S. homes for a year)
  • Obtained through hydrolysis of heavy water (water with deuterium) which splits water molecules into oxygen and deuterium gas

Tritium

  • Naturally occurring tritium is rare (global inventory is around 20 kg)
  • Can be bred from lithium, an abundant resource (the ability to do this within the fusion reaction is important for large scale fusion power)

Fusion Fuel is Extremely Energy Dense*

14,000,000x
more energy dense than coal

6,000,000x
more energy dense than natural gas

4x
more energy dense than fission

*Energy densities measured by weight


Net Energy Production

The variable Q represents the fusion energy gain factor, which is the ratio of produced energy to injected energy.

$$Q = {produced\hspace{9px}energy \over injected\hspace{9px}energy}$$

We want Q > 1. Different levels of Q help us measure our progress toward commercial fusion. The levels are based on how we define the system.

$$Scientific\hspace{7px}Q\hspace{7px}(Q_{sci}) = {fusion\hspace{7px}energy \over energy\hspace{7px}delivered\hspace{7px}to\hspace{7px}the\hspace{5px}fusion\hspace{7px}target\hspace{7px} (e.g.,\hspace{4px}energy\hspace{7px}from\hspace{7px}lasers)}$$

$$Engineering\hspace{7px}Q\hspace{7px}(Q_{eng}) = {electricity\hspace{7px}to\hspace{7px}the\hspace{7px}grid \over electricity\hspace{7px}needed\hspace{7px}to\hspace{7px}run\hspace{7px}the\hspace{7px}entire\hspace{7px}power\hspace{7px}plant}$$

Qsci > 1 has recently been achieved

First Time

Qsci = 1.5
achieved by the National Ignition Facility (NIF) in Livermore, CA in December 2022

Highest Value

Qsci = 4.13
achieved by the NIF in April 2025

Required for commercial fusion

Qeng > 1
much more difficult to achieve than Qsci > 1


Conditions for Fusion to Occur

The Fusion Triple Product (related to the Lawson Criteria) is a convenient metric for how close a plasma* is to energy breakeven once nuclei are in the plasma state.

temperature × confinement time × plasma density > 10 21 keV s m-3

Temperature

Fusion reactions on Earth require extremely high temperatures
>100 million degrees Celsius
to put the reactants into the plasma state and overcome electrostatic forces between the nuclei to force the nuclei to fuse.

That's over 6x the temperature of the core of the sun. The sun is massive, which allows the center (where fusion occurs) to have high pressures we can't replicate on Earth. That means we must compensate by going even higher in temperature.

Confinement and Plasma Density

No solid known material on Earth is capable of physically confining plasma at >100 million degrees. That means a confinement system that doesn’t allow the plasma to touch the walls must hold the plasma in place.

*Plasmaa state of matter in which gases become ionized as atoms shed their electrons, creating an electrically charged gas with free electrons and ions


Most Common Approaches to Fusion

Gravitational confinement (like the sun uses) is not an option on Earth. The two most common approaches to fusion on Earth are magnetic and inertial confinement.

Magnetic Confinement

Uses powerful magnetic fields to confine the plasma:

  • Requires relatively low plasma density and long energy confinement times (seconds)
  • The tokamak is the most researched magnetic confinement design and has the most global funding of all fusion designs
Tokamak schematic
Tokamak schematic: donut-shaped, magnetized fusion machine

Inertial Confinement

Creates plasma and fusion with very quick bursts of energy imploding a fuel-filled target, typically using high-powered lasers:

  • Requires high plasma density over a very short period (nanoseconds)
  • An inertial confinement experiment holds the world record for fusion energy gain relative to energy delivered to the fusion target
Cross-section of hohlraum with lasers and fuel pellet
One type of inertial confinement fusion: indirect drive, where high-powered lasers hit the insides of the hohlraum and generate x-rays that compress the fuel


There are many other fusion approaches being pursued by private companies or that have been theorized (e.g., a combination of magnets and lasers, electric currents to induce a magnetic field, electrons to induce an electric field).


Leading Fusion Endeavors

World

50+ Countries

involved in research on plasma physics and nuclear energy technology development

ITER

33 countries collaborating to build the world's largest fusion machine

50+ Private Companies

in the fusion space

>$9.7 billion

total investment to date in private fusion companies

U.S.

9 National Labs

engaged in fusion research

50+ Universities

conducting fusion research

29 Private Companies

in the fusion space

$1.4 billion

total investment in public-private partnerships, national labs, and universities from U.S. government in 2024

China was a late entrant into the nuclear fusion industry but is now investing $1.5 billion dollars per year and making rapid progress in fusion technology development.


Drivers

  • The fuel is abundant (nearly inexhaustible); deuterium is common in seawater, and tritium can be bred from lithium during the fusion reaction
  • No long-lived radioactive waste; the product of fusion reactions is helium
  • No air emissions like GHGs, particles, etc.
  • Super energy dense; net energy production is about 4 times that of fission
  • Safety: unlike with nuclear fission, runaway reactions in a fusion plant are not possible. If something were to go wrong, the temperature of the plasma would decrease, the plasma would extinguish, and fusion reactions would cease

Barriers

  • Technology is in the research phase
  • Very energy intensive to get the fusion reaction going; reactor needs to produce more energy than what is put into it
  • Fusion reactions are not yet self-sustaining
  • Containment: no solid known material on Earth capable of physically confining plasma at >100 million degrees
  • Regulatory approval
  • Cost: fusion research is very expensive

Climate Impact: Low

Low gradient
  • Zero operating emissions

Environmental Impact: Low

Low gradient
  • No air pollution
  • No high-level radioactive waste
  • Some low-level radioactive waste that must be safely stored

 

Updated August 2025

Our 10-Minute Take On
Fusion

If you're short on time, start by watching this video of key highlights from our lecture on Nuclear Fusion.

Diana Gragg

Presented by: Diana Gragg, PhD; Core Lecturer, Civil and Environmental Engineering, Stanford University; Explore Energy Managing Director, Precourt Institute for Energy
 

Recorded: June 6, 2025  
Duration: 8 minutes

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If you liked this video, watch the other 10-Minute Takes here!

Before You Watch Our Lecture on
Fusion

We assign videos and readings to our Stanford students as pre-work for each lecture to help contextualize the lecture content. We strongly encourage you to review the Essential videos and readings before watching our lecture on Fusion Energy. Include selections from the Optional and Useful list based on your interests and available time. 

Essential

Optional and Useful

Our Lectures on
Fusion

These are our Stanford University Understand Energy course lectures on fusion. We strongly encourage you to watch the full lecture to understand the potential role of fusion in our energy system and to be able to put this complex topic into context. For a complete learning experience, we also encourage you to watch / read the Essential videos and readings we assign to our students before watching the lecture.

Lecture 1: An Overview of Fusion Energy: Igniting a New Energy Era with Commercial Fusion Power

Clea Kolster

Presented by: Clea Kolster, PhD; Partner and the Head of Science, Lowercarbon Capital
Recorded on: May 28, 2025   Duration: 39 minutes

Table of Contents

(Clicking on a timestamp will take you to YouTube.)
00:00 Introduction 
03:48 What is Fusion? 
05:27 Fusion Fuels 
07:27 How to Harness Fusion Energy 
10:03 Who is Working on Fusion? 
13:12 Types of Reactors 
30:45 Q & A

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Lecture 2: Harnessing Star-Power — The Frontier of Matter at Extreme Conditions

Headshot of Arianna Gleason

Presented by: Arianna Gleason, Senior Scientist, SLAC National Accelerator Laboratory
Recorded on: September 9, 2025   Duration: 28 minutes

Table of Contents

(Clicking on a timestamp will take you to YouTube.)
00:00 Introduction
8:00 Fusion energy to meet growing demand
10:05 Example fusion research at SLAC
25:22 Closing thoughts

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Printable PDF: Questions, Answer Key

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Fusion

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