Nuclear Energy
Chapter Name : Nuclei |
Sub Topic Code : 101_12_13_07_05 |
Topic Name : Nuclear Energy |
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Sub Topic Name : Controlled Thermonuclear Fusion |
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Introduction
Thermonuclear fusion is a way to achieve nuclear fusion by using extremely high temperatures.
Pre-Requisites:
Thermonuclear Fusion
Activity:
Sun and the stars.
Real Life Question:
What is nuclear fusion?
Key Words / FlashCards
| Key Words | Definitions (pref. in our own words) |
|---|---|
| Nuclear fusion | Nuclear fusion is a nuclear reaction in which two or more atomic nuclei collide at very high speed and join to form a new type of atomic nucleus. |
Learning aids / Gadgets
| Gadgets | How it can be used |
|---|---|
| Deuterium–tritium fusion reaction | The energy necessary to overcome the Coulomb barrier is 0.1 MeV. Converting the units between electronvolts and kelvin shows that the barrier would be overcome at a temperature in excess of 120 million kelvins. |
Real life uses :
Gravitational confinement.
Places to visit :
Solar observatory.
Practical examples around us
| Examples | Explainations |
|---|---|
| Thermonuclear fusion | If the matter is sufficiently heated (hence being plasma), the fusion reaction may occur due to collisions with extreme thermal kinetic energies of the particles. This process is called the thermonuclear fusion, and is the only one which seems to be useful for obtaining fusion energy. |
What you learn in Theory:
The energy generation rate in the core of a star balances the gravitational force of the material in the star. A more massive star generates more energy, thereby holding itself up.
What you learn in Practice:
If the energy generation rate is too high, then the luminosity produced in the core Lc is too great, and the core expands, subsequently cooling, and thus restoring the proper rate of energy production.