Linked from

The 14 pages that link to Radiative cooling, each with the reason it gives.

• Star formationRelated: Cooling lowers gas pressure, allowing gravity to compress cloud material more readily.

• Thermal radiationRelated: It uses outgoing thermal radiation to lower an object's temperature.

• Stefan–Boltzmann lawRelated: Its temperature-dependent emission follows the law, modified by emissivity and surroundings.

• EmissivityRelated: High emissivity in selected infrared bands enables surfaces to shed heat efficiently.

• Kirchhoff's law of thermal radiationRelated: The law constrains how a designed emitter's spectral absorptivity relates to its emission.

• Inverse Compton scatteringRelated: Energy given to photons cools the relativistic electrons that drive the scattering.

• Circumgalactic mediumRelated: Cooling lets hot circumgalactic gas condense and potentially return to the galaxy.

• Disk instabilityRelated: A disk must shed heat quickly enough for a gravitationally compressed region to remain bound.

• Coronal heating problemRelated: Coronal radiation removes energy that any heating process must continually replace.

• Frost protectionRelated: Clear nights can cool crops below air temperature through radiative heat loss.

• Katabatic windRelated: Clear-sky surface heat loss cools air in contact with slopes, making it denser.

• FrostRelated: Clear skies let surfaces radiate heat away and cool below the surrounding air.