Classical thermodynamics, heat transfer Thermal radiation Concept
Black body
Summary
A black body is an idealised body that absorbs all electromagnetic radiation that falls on it, at every wavelength and from every direction. In equilibrium at a given temperature, no body emits more thermal radiation than it does. Its spectrum is given by Planck's law. Its total emitted power follows the Stefan–Boltzmann law, and real surfaces are described by comparing them with it through their emissivity. The study of black-body radiation led Planck to the quantum hypothesis.
Where this leads
15 pages build on this one.
- Energy balance model
- Rosseland mean opacity
- Stefan–Boltzmann law
- Radiosity
- Radiative heat transfer in participating media
- Sunyaev–Zeldovich effect
- Rosseland approximation
- Kirchhoff's law of thermal radiation
- Wien's displacement law
- Rayleigh–Jeans law
- Planck's law
- Lambert's cosine law
- Emissivity
- Effective temperature
- Yarkovsky effect
Further reading
About this page
| Tag | A2RMYX8A65 |
|---|---|
| URI | m2://A2RMYX8A65 |
| Kind | concept |
| Writing | W0 stub |
| MSC | 80A21, 78A40 |
| Same as | |
| Changed | 3 November 2026 |
Markdown · JSON · Edit on GitHub
What this page needs for W1
- an inventory row: the row of the inventory that the node accounts for (0 of 1)
- a source with a locator (0 of 1)
The writing levels say how complete the text of a page is. They do not measure its truth.
What links here
Definitions
Used by
- Rosseland mean opacity
- Stefan–Boltzmann law
- Radiosity
- Radiative heat transfer in participating media
- Sunyaev–Zeldovich effect
- Rosseland approximation
- Kirchhoff's law of thermal radiation
- Wien's displacement law
- Rayleigh–Jeans law
- Planck's law
- Lambert's cosine law
- Emissivity
- Effective temperature
- Yarkovsky effect