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One may assume that the planet radiates energy like a blackbody at some temperature according to the Stefan–Boltzmann law. Thermal equilibrium exists when the power supplied by the star is equal to the power emitted by the planet. The temperature at which this balance occurs is the planetary equilibrium temperature. [4] [5] [6]
If Earth were frozen entirely (and hence be more reflective), the average temperature of the planet would drop below −40 °C (−40 °F). [17] If only the continental land masses became covered by glaciers, the mean temperature of the planet would drop to about 0 °C (32 °F). [18]
The planet has a negligible atmospheric greenhouse, so its surface temperature is simply determined by... [the hypothetical star's] luminosity and its [the planet's] overall albedo [reflective power, the fraction of incident radiation reflected by the surface], which is, in turn, influenced by the coverage of the two daisy types. [4]
The Bond albedo (also called spheric albedo, planetary albedo, and bolometric albedo), named after the American astronomer George Phillips Bond (1825–1865), who originally proposed it, is the fraction of power in the total electromagnetic radiation incident on an astronomical body that is scattered back out into space.
The planets are solar thermal collectors on a large scale. The temperature of a planet's surface is determined by the balance between the heat absorbed by the planet from sunlight, heat emitted from its core, and thermal radiation emitted back into space. Emissivity of a planet is determined by the nature of its surface and atmosphere. [11]
Sudarsky's classification of gas giants for the purpose of predicting their appearance based on their temperature was outlined by David Sudarsky and colleagues in the paper Albedo and Reflection Spectra of Extrasolar Giant Planets [1] and expanded on in Theoretical Spectra and Atmospheres of Extrasolar Giant Planets, [2] published before any successful direct or indirect observation of an ...
[3] [4] [5] The planet is idealized by the model as being functionally "layered" with regard to a sequence of simplified energy flows, but dimensionless (i.e. a zero-dimensional model) in terms of its mathematical space. [6] The layers include a surface with constant temperature T s and an atmospheric layer with constant temperature T a. For ...
The effective temperature of the Sun (5778 kelvins) is the temperature a black body of the same size must have to yield the same total emissive power.. The effective temperature of a star is the temperature of a black body with the same luminosity per surface area (F Bol) as the star and is defined according to the Stefan–Boltzmann law F Bol = σT eff 4.