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\@writefile{toc}{\contentsline {section}{\numberline {1}\bf  The Volcanoes of Io}{1}}
\@writefile{toc}{\contentsline {subsection}{\numberline {1.1}Introduction}{1}}
\@writefile{toc}{\contentsline {subsection}{\numberline {1.2}Introduction to Io}{1}}
\@writefile{lof}{\contentsline {figure}{\numberline {1}{\ignorespaces Left: The four Galilean moons of Jupiter. Right: An erupting volcano on Io seen in a Voyager image.}}{2}}
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\@writefile{lof}{\contentsline {figure}{\numberline {2}{\ignorespaces Left: Because Io's orbit around Jupiter is an ellipse, the distance is constantly changing, and so is the gravitational force exerted on Io by Jupiter (note that this figure is not to scale, and the ellipticity of the orbit and the shape of Io have been grossly exaggerated to demonstrate the effect). This changing force causes Io to stretch and relax over each orbit. Right: The tidal forces exerted by Europa and Ganymede distort the orbit of Io because the orbits of all three moons are in ``resonance'': for every four trips Io makes around Jupiter, Europa makes two, and Ganymede makes one. This resonance enhances the gravitational forces of Europa and Ganymede, as these three moons keep returning to the same (relative) places on a regular basis. This repeated and periodic tugging on Io causes its orbit to be much more eccentric than it would be if Europa and Ganymede did not exist. }}{3}}
\newlabel{tidal}{{2}{3}}
\@writefile{toc}{\contentsline {subsection}{\numberline {1.3}The Electromagnetic Spectrum}{3}}
\@writefile{lof}{\contentsline {figure}{\numberline {3}{\ignorespaces The wavelength is the distance between two crests.}}{4}}
\newlabel{wavelength}{{3}{4}}
\@writefile{lof}{\contentsline {figure}{\numberline {4}{\ignorespaces The electromagnetic spectrum.}}{4}}
\newlabel{em}{{4}{4}}
\@writefile{toc}{\contentsline {subsection}{\numberline {1.4}Blackbody Radiation Review}{4}}
\@writefile{lof}{\contentsline {figure}{\numberline {5}{\ignorespaces The spectra of blackbodies always have the same shape, but the wavelength where the {\it  peak emission} occurs depends on temperature, and can be calculated using the ``Wien displacement law'' (since Wien is a German name, it is properly pronounced ``Veen''). In this particular plot the unit of wavelength is the micrometer, 10$^{\rm  -6}$ meter, symbolized by ``$\mu $m.'' Note also that the x-axis is plotted as the {\it  log} of wavelength, and the y-axis is the {\it  log} of the radiant energy. We have to use this type of ``log-log'' plot since blackbodies cover a large range in radiant energy and wavelength, and we need an efficient way to compress the axes to make compact plots. We will be using these types of plots for the volcanoes of Io.}}{5}}
\newlabel{bbody}{{5}{5}}
\@writefile{toc}{\contentsline {subsection}{\numberline {1.5}Simulating Tidal Heating}{9}}
\@writefile{lot}{\contentsline {table}{\numberline {1}{\ignorespaces Exercise Ball Temperatures}}{10}}
\newlabel{exercise}{{1}{10}}
\@writefile{toc}{\contentsline {subsection}{\numberline {1.6}Investigating the Volcanoes of Io}{10}}
\@writefile{lof}{\contentsline {figure}{\numberline {6}{\ignorespaces The energy vs. wavelength, the ``spectra'' (spectra is plural of spectrum), produced by two blackbodies with different temperatures.}}{12}}
\newlabel{2bbody}{{6}{12}}
\@writefile{lot}{\contentsline {table}{\numberline {2}{\ignorespaces Region \#2 Box Temperatures}}{14}}
\newlabel{region2tab}{{2}{14}}
\@writefile{lof}{\contentsline {figure}{\numberline {7}{\ignorespaces The blackbody spectra of the six boxes shown in Image \#7. Be careful, these plots have {\it  log} wavelength on the x-axis.}}{16}}
\newlabel{loki}{{7}{16}}
\@writefile{toc}{\contentsline {subsection}{\numberline {1.7}Take-Home Exercise (35 points total)}{18}}
\@writefile{toc}{\contentsline {subsection}{\numberline {1.8}Possible Quiz Questions}{21}}
\@writefile{toc}{\contentsline {subsection}{\numberline {1.9}Extra Credit (ask your TA for permission before attempting, 5 points)}{21}}