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翻訳と辞書　辞書検索 [ 開発暫定版 ] スポンサード リンク Planetary equilibrium temperature ： ウィキペディア英語版 Planetary equilibrium temperature The planetary equilibrium temperature is a theoretical temperature that a planet would be at when considered simply as if it were a black body being heated only by its parent star. In this model, the presence or absence of an atmosphere (and therefore any greenhouse effect) is not considered, and one treats the theoretical black body temperature as if it came from an idealized surface of the planet. Other authors use different names for this concept, such as equivalent blackbody temperature of a planet,〔Wallace, J.M., Hobbs, P.V. (2006). ''Atmospheric Science. An Introductory Survey'', second edition, Elsevier, Amsterdam, ISBN 978-0-12-732951-2. Section 4.3.3, pp. 119–120.〕 or the effective radiation emission temperature of the planet.〔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.〕 Similar concepts include the global mean temperature, global radiative equilibrium, and global-mean surface air temperature,〔Wallace, J.M., Hobbs, P.V. (2006). ''Atmospheric Science. An Introductory Survey'', second edition, Elsevier, Amsterdam, ISBN 978-0-12-732951-2., p.444.〕 which includes the effects of Global warming. ==Calculation of blackbody temperature== If the incident solar radiation ("insolation") on the planet at its orbital distance from the Sun is Io, the amount of energy absorbed by the planet will depend on its albedo and its cross-sectional area: $\_=\; \backslash left(\; 1-a\; \backslash right)\; \backslash pi\; \}^$ The infrared power radiated by the planet as thermal radiation will depend on its emissivity and its surface area, according to the Stefan–Boltzmann equation: $\_=\; \backslash epsilon\; \backslash sigma\; A\; ^$ where Pout is the radiated power, $\backslash epsilon$ is the emissivity, σ the Stefan–Boltzmann constant, A the surface area, and T the temperature. For a spherical planet, the surface area $A\; =\; 4\backslash pi\; \}^$ The equilibrium temperature is then calculated by setting Pin=Pout for the case of a blackbody, in which the emissivity $\backslash epsilon$ = 1. Thus, $\_=\; \}\backslash right)\}^$ 抄文引用元・出典: フリー百科事典『 ウィキペディア（Wikipedia）』 ■ウィキペディアで「Planetary equilibrium temperature」の詳細全文を読む スポンサード リンク 翻訳と辞書 : 翻訳のためのインターネットリソース Copyright(C) kotoba.ne.jp 1997-2016. All Rights Reserved.