Editing Effective temperature (section)

{{Short description|Temperature of a black body that would emit the same total amount of electromagnetic radiation}}
The '''effective temperature''' <!-- or '''effective radiative emission temperature''' failed to find in references -->of a body such as a star or planet is the [[temperature]] of a [[black body]] that would emit the same total amount of [[electromagnetic radiation]].<ref name="Archie2003">{{cite book | title = Astronomy | author = Archie E. Roy, David Clarke | publisher = [[CRC Press]] | date = 2003 | isbn = 978-0-7503-0917-2 | url = https://books.google.com/books?id=v2S6XV8dsIAC&pg=PA216 }}</ref><ref>Stull, R. (2000). ''Meteorology For Scientists and Engineers. A technical companion book with Ahrens' Meteorology Today'', Brooks/Cole, Belmont CA, {{ISBN|978-0-534-37214-9}}, p. 400.</ref>  Effective temperature is often used as an estimate of a body's surface temperature when the body's [[emissivity]] curve (as a function of [[wavelength]]) is not known.

When the star's or planet's net [[emissivity]] in the relevant wavelength band is less than unity (less than that of a [[black body]]), the actual temperature of the body will be higher than the effective temperature.  The net emissivity may be low due to surface or atmospheric properties, such as the [[greenhouse effect]].