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In astronomy, air mass (or airmass) is the optical path length through Earth’s atmosphere for light from a celestial source. As it passes through the atmosphere, light is attenuated by scattering and absorption; the more atmosphere through which it passes, the greater the attenuation. Consequently, celestial bodies at the horizon appear less bright than when at the zenith. The attenuation, known as atmospheric extinction, is described quantitatively by the Beer–Lambert–Bouguer law. “Air mass” normally indicates ''relative air mass'', the path length relative to that at the zenith at sea level so, by definition, the sea-level air mass at the zenith is 1. Air mass increases as the angle between the source and the zenith increases, reaching a value of approximately 38 at the horizon. Air mass can be less than one at an elevation greater than sea level; however, most closed-form expressions for air mass do not include the effects of elevation, so adjustment must usually be accomplished by other means. In some fields, such as solar energy and photovoltaics, air mass is indicated by the acronym AM; additionally, the value of the air mass is often given by appending its value to AM, so that AM1 indicates an air mass of 1, AM2 indicates an air mass of 2, and so on. The region above Earth’s atmosphere, where there is no atmospheric attenuation of solar radiation, is considered to have “air mass zero” (AM0). Tables of air mass have been published by numerous authors, including Bemporad (1904), Allen (1976),〔 Allen’s air mass table was an abbreviated compilation of values from earlier sources, primarily Bemporad (1904). 〕 and Kasten and Young (1989). ==Calculating air mass== 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「Air mass (astronomy)」の詳細全文を読む スポンサード リンク
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