This law states that the total amount of radiant energy (including all frequencies) emitted per unit time from a unit surface area of a blackbody at various temperatures is proportional to the fourth power of the blackbody's absolute temperature T, and is expressed as σT 4 (when σ is calculated using Planck's radiation law, it is given as σ=5.67×10(-/) 1 2 watt・cm(-/) 2・deg(-/) 4 ). It was discovered by Stephan (1879) and theoretically proven by Boltzmann (1884). It is used to measure high temperatures. →Wien's Displacement Law→Related topics: Cavity radiation | Blackbody radiation | Radiation pyrometer Source : Heibonsha Encyclopedia About MyPedia Information |
いろいろな温度の黒体の単位表面積から単位時間に放出される放射エネルギーの総量(すべての振動数を含む)は,黒体の絶対温度Tの4乗に比例し,σT4(プランクの放射法則によってσを計算すると,σ=5.67×10(-/)12watt・cm(-/)2・deg(-/)4)で表されるという法則。シュテファンが発見(1879年),ボルツマンが理論的に証明(1884年)。高温測定に利用される。→ウィーンの変位則 →関連項目空洞放射|黒体放射|放射高温計 出典 株式会社平凡社百科事典マイペディアについて 情報 |
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