Emissivity
- Stars are good approximations to a black body, whereas planets are not
- This can be quantified using the emissivity
- Emissivity, e, is defined as
The the ratio of the power radiated per unit area by a surface compared to that of a black body at the same temperature
- It can be calculated using the equation
e =
- Calculations of the emissivity assume that the black body:
- Is at the same temperature as the object
- Has the same dimensions as the object
- For a perfect black body, emissivity is equal to 1
- When using the Stefan-Boltzmann law for an object which is not a black body, the equation becomes:
P = eσAT4
- Where:
- P = total power emitted by the object (W)
- e = emissivity of the object
- σ = the Stefan-Boltzmann constant
- A = total surface area of the object black body (m2)
- T = absolute temperature of the body (K)
Exam Tip
You will be expected to remember that a perfect black body has an emissivity of 1 - this information is not included in the data booklet!