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diff --git a/blackbody_new.tex b/blackbody_new.tex index d6124de..e892162 100644 --- a/blackbody_new.tex +++ b/blackbody_new.tex @@ -216,7 +216,7 @@ S_{det}(r)=\frac{P_0}{2\pi r^2} \newpage \section*{Universal thermometer} -Blackbody radiation gives us an ability to measure the temperature of remote objects. Have you ever asked yourself how do astronomer know the temperature of stars or other objects many light years away? The answer - by measuring the light they emit and analyzing its spectrum conposition using the expressions for the blackbody radiation spectrum. Wein's law Eq.(\ref{weins}) links the wavelength at which the most radiation is emitted to the inverse of the object's temperature, thus the colder stars emit predominantly in red (hence the name ``red giants''), while emission pick for hot young stars is shifted to the blue, making them emit in all visible spectrum. +Blackbody radiation gives us an ability to measure the temperature of remote objects. Have you ever asked yourself how do astronomer know the temperature of stars or other objects many light years away? The answer - by measuring the light they emit and analyzing its spectrum composition using the expressions for the blackbody radiation spectrum. Wein's law Eq.(\ref{weins}) links the wavelength at which the most radiation is emitted to the inverse of the object's temperature, thus the colder stars emit predominantly in red (hence the name ``red giants''), while emission pick for hot young stars is shifted to the blue, making them emit in all visible spectrum. \begin{figure}[h] \centering \includegraphics[height=2.5in]{./pdf_figs/blackbody_radn_curves} |