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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.
:\Sigma_ \propto (\Sigma_)^n.
In general the SFR surface density (\Sigma_) is in units of solar masses per year per square parsec (M_\odot ~\textrm^ \textrm^) and the gas surface density in grams per square parsec (\textrm~\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 \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 \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)
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