Version: 1.0 (using KDE 3.2.0 RC1, SuSE) Compiler: gcc version 3.3.1 (SuSE Linux) OS: Linux (i686) release 2.4.21-166-athlon Hi, look at string 19 and 20 of kstars_blackbody.po: "Five years later, Austrian physicist Ludwig Boltzman derived the same equation and is now known as the Stephan-Boltzman law. If we assume a spherical star with radius R, then the luminosity of such a star is" "where R is the star radius in cm, and the alpha is the Stephan- Boltzman constant, which has the value:" The law is named after Stephan Josef Stefan and Ludwich Boltzman. So the law should be named Stefan-Boltzman, not Stephan-Boltzman Rinse
Subject: kdeedu/doc/kstars CVS commit by harris: Fixing three bugs in blackbody.docbook: 73930: Misspelled "Wien's Law" 73931: Incomplete phrase: actually, this phrase is not incomplete. If you look at the handbook, you'll see that the last part of the sentence is an equation presented as an image in the document. However, to make the sentence a bit clearer, I have changed it to: "For example, the sun has an average temperature of 5800 K, so its wavelength of maximum emission is given by:" 73932: Misspelled "Stefan-Boltzmann Law" CCMAIL: 73930-done@bugs.kde.org CCMAIL: 73931-done@bugs.kde.org CCMAIL: 73932-done@bugs.kde.org M +6 -6 blackbody.docbook 1.9 --- kdeedu/doc/kstars/blackbody.docbook #1.8:1.9 @@ -96,6 +96,6 @@ <para> -where T is the temperature in Kelvin. Wein's law (also known as -Wein's displacement law) states that the +where T is the temperature in Kelvin. Wien's law (also known as +Wien's displacement law) states that the wavelength of maximum emission from a blackbody is inversely proportional to its temperature. This makes sense; @@ -106,6 +106,6 @@ <para> -For example, the sun has an average temperature of 5800 K with a -wavelength of maximum emission equal to +For example, the sun has an average temperature of 5800 K, so +its wavelength of maximum emission is given by: <mediaobject> @@ -145,5 +145,5 @@ <para> Five years later, Austrian physicist Ludwig Boltzman derived the same -equation and is now known as the Stephan-Boltzman law. If we assume a +equation and is now known as the Stefan-Boltzman law. If we assume a spherical star with radius R, then the luminosity of such a star is </para> @@ -159,5 +159,5 @@ <para> where R is the star radius in cm, and the alpha is the -Stephan-Boltzman constant, which has the value: +Stefan-Boltzman constant, which has the value: <mediaobject>