Fusion (Physics)

Introduction

Fusion is a fundamental nuclear process in which two atomic nuclei combine to form a nucleus with a larger mass number.

Nuclear Fusion: Fusion involves the merging of atomic nuclei to create a nucleus of higher mass.
Stellar Fusion: Fusion is the primary nuclear process that powers stars like the Sun, where hydrogen nuclei combine to form helium nuclei.
Energy Release: Fusion reactions release a substantial amount of energy in the form of kinetic energy.
E=mc²: Albert Einstein's famous equation, E=mc², demonstrates the equivalence of mass and energy, where energy (E) is related to mass (m) by the speed of light (c).

Fusion Process Diagram

In nuclear fusion, two atomic nuclei, often hydrogen isotopes, collide and fuse to create a new, heavier nucleus.
For example, the fusion of hydrogen-1 and hydrogen-2 nuclei forms helium-3.

Stellar Fusion Diagram

Fusion reactions are the primary energy source for stars like the Sun.
In the Sun's core, hydrogen nuclei combine to form helium through a series of fusion reactions, releasing vast amounts of energy in the form of light and heat.

Fusion reactions release energy in the form of kinetic energy of the resulting nucleus and emitted particles.
This energy can be harnessed for various applications, including the development of advanced energy sources.

Diagram

Albert Einstein's equation, E=mc², states that energy (E) is proportional to mass (m) and the square of the speed of light (c).
It highlights the concept that mass can be converted into energy and vice versa, illustrating the immense energy potential in fusion reactions.

Fusion is a nuclear process where two atomic nuclei combine to create a nucleus with a higher mass number.
Fusion reactions are the main source of energy in stars like the Sun.
Fusion reactions release energy, which can be harnessed for various applications.
Albert Einstein's equation, E=mc², demonstrates the relationship between mass and energy, emphasising the significant energy potential of fusion.