Published by Patrick Mutisya · 14 days ago
Nuclear fusion is the process in which two light atomic nuclei combine to form a heavier nucleus. During this process a small amount of the total mass is converted into a large amount of energy.
The Sun’s core is extremely hot (≈ \$1.5\times10^{7}\,\text{K}\$) and under immense pressure. These conditions allow hydrogen nuclei (protons) to overcome their electrostatic repulsion and fuse together.
The dominant fusion process in the Sun is the proton–proton (p‑p) chain, which can be summarised in three main steps.
\$\mathrm{^{1}H} + \mathrm{^{1}H} \rightarrow \mathrm{^{2}H} + e^{+} + \nu_{e}\$
\$\mathrm{^{2}H} + \mathrm{^{1}H} \rightarrow \mathrm{^{3}He} + \gamma\$
\$\mathrm{^{3}He} + \mathrm{^{3}He} \rightarrow \mathrm{^{4}He} + 2\,\mathrm{^{1}H}\$
The total mass of the four original protons is slightly greater than the mass of the resulting helium‑4 nucleus. The missing mass \$\Delta m\$ is converted into energy according to Einstein’s equation:
\$E = \Delta m\,c^{2}\$
For the complete p‑p chain the energy released is about \$26.7\ \text{MeV}\$ per helium‑4 nucleus formed, which corresponds to \$4.3\times10^{-12}\ \text{J}\$.
The Sun’s fusion provides a continuous, renewable source of energy that reaches Earth as sunlight. Understanding fusion helps explain why solar power is a viable, sustainable energy resource.
| Step | Reactants | Products | Energy Released (MeV) |
|---|---|---|---|
| 1 | \$\mathrm{^{1}H} + \mathrm{^{1}H}\$ | \$\mathrm{^{2}H} + e^{+} + \nu_{e}\$ | 0.42 |
| 2 | \$\mathrm{^{2}H} + \mathrm{^{1}H}\$ | \$\mathrm{^{3}He} + \gamma\$ | 5.49 |
| 3 | \$\mathrm{^{3}He} + \mathrm{^{3}He}\$ | \$\mathrm{^{4}He} + 2\,\mathrm{^{1}H}\$ | 12.86 |
| Total per helium‑4 nucleus | 26.7 | ||