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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 Kennicutt-Schmidt Law ： ウィキペディア英語版 Kennicutt–Schmidt law In astronomy, the Kennicutt–Schmidt Law (or simply Schmidt Law) is an empirical relation between the gas density and star formation rate (SFR) in a given region. The relation was first examined by Maarten Schmidt in a 1959 paper in which he proposed that the SFR surface density scales as some positive power $n$ of the local gas surface density.〔 i.e. :$\backslash Sigma\_\; \backslash propto\; (\backslash Sigma\_)^n$. In general the SFR surface density $(\backslash Sigma\_)$ is in units of solar masses per year per square parsec $(M\_\backslash odot\; ~\backslash textrm^\; \backslash textrm^)$ and the gas surface density in grams per square parsec $(\backslash textrm~\backslash textrm^)$. Using an analysis of gaseous helium and young stars in the solar neighborhood, the local density of white dwarfs and their luminosity function, and the local helium density, Schmidt suggested a value of $n\; \backslash approx\; 2$ (and very likely between 1 and 3). All of the data used were gathered from the Milky Way, and specifically the solar-neighborhood. More recently, Robert Kennicutt examined the connection between gas density and SFR for nearly 100 nearby galaxies to estimate a value of $n\; =\; 1.4\; \backslash pm\; 0.15$.〔 ==References== 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「Kennicutt–Schmidt law」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.