Radiative correction - bolometric correction

Japanese: 放射補正量 - ほうしゃほせいりょう（英語表記）bolometric correction

The difference between the radiant magnitude of a star's brightness and its absolute apparent magnitude. Since the apparent magnitude is a color distribution close to the sensitivity of the eye, stars with a similar energy distribution require less correction. For hot or cold stars, there is a lot of radiation at wavelengths that are out of the sensitivity distribution of the eye, so the radiant magnitude becomes brighter and requires negative correction. In other words, it is a function of the spectral type and luminosity function, or in other words, the effective temperature and surface gravity. The value for the sun is -0.08 magnitude. [Masayuki Kondo]

Source: Heibonsha World Encyclopedia, 2nd Edition Information

Japanese:

星の明るさの放射等級と絶対実視等級の差。実視等級は目の感度に近い色分布なので，エネルギー分布がそれに近い星では補正が少ない。高温または低温の星では，目の感度分布からずれた波長で放射が多いので，放射等級が明るくなり，負の補正を必要とする。つまりスペクトル型と光度関数，別のことばでは有効温度と表面重力の関数である。太陽の値は－0.08等。【近藤雅之】

出典　株式会社平凡社世界大百科事典第２版について　情報

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