Blackbody total emission
Thermal equilibrium fixes an ideal absorber's total emitted power.
Key knowledge
An ideal blackbody at temperature T emits total radiant power per area M = σT⁴, integrated over outgoing directions and all wavelengths.
Values and equations
M = P/A = σT⁴
- M
- Radiant exitance W m⁻²
- P
- Emitted power W
- A
- Emitting area m²
- T
- Absolute temperature K
- σ
- Stefan–Boltzmann constant W m⁻² K⁻⁴
Conditions and scope
- T is absolute temperature; M is emitted power, not net exchange with surroundings.
- Real spectral emissivity and radiative surroundings need additional treatment.
Sources · 1
References
Sources retain their recorded scope. A source link alone does not establish verification of every statement.
Evidence and review
Equation 6.4, total spectral power and area/temperature definitions.
2026-10-10 · Integrated ideal-blackbody Stefan–Boltzmann emission only; fitted temperatures and current constants not tabulated.
Entry details
Permanent link to this entry ↗- Record identity
- physics-blackbody-radiation
- Revision
- university-reference.1
- Structured reference record
- University reference · University core expansion