Exercise 1.2.26

Question

Astronomers infer the radiant exitance (radiant flux emitted per unit area) of stars using the Stefan Boltzmann Law:
    $$E(T)= (5.67 	imes 10^{-8})T^4,$$
    where $E$ is the energy radiated per unit of surface area measured in watts (W) and $T$ is the absolute temperature measured in kelvins (K).
    \begin{enumerate}[label=(\alph*)]
        \item Graph the function $E$ for temperatures T between 100 K and 300 K.
        \item Use the graph to describe the change in energy $E$ as the temperature $T$ increases.
    \end{enumerate}

Khagan Gulusoy · Accepted Answer

\begin{enumerate}[label=(\alph*)]
    \item \begin{figure}[H] \centering
    \begin{tikzpicture}
    \begin{axis}[axis lines=left, xmin=0, xmax=300, ymax=460, ymin=0, xlabel={$T$}, ylabel={$E(T)$}, x label style = {at={(ticklabel cs:0.9)},anchor=south,above=10mm}, y label style={anchor=north, above=3mm}]
         \addplot[domain=100:300, samples=50, mark=none, color=blue, ultra thick] {5.67*10^(-8)*x^4};
    \end{axis}    
    \end{tikzpicture}
    \end{figure}
    \item At first, there is a gradual increase in energy. After that, the change in energy begins to increase significantly. It is apparent that the graph represents a portion of an even power function.
\end{enumerate}

Exercise 1.2.26

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Exercise 1.2.26

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