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\@writefile{toc}{\contentsline {section}{\numberline {1}\bf  Characterizing Exoplanets}{1}}
\@writefile{toc}{\contentsline {subsection}{\numberline {1.1}Introduction}{1}}
\@writefile{toc}{\contentsline {section}{\numberline {2}Types of Exoplanets}{1}}
\@writefile{toc}{\contentsline {subsection}{\numberline {2.1}Gas Giants}{1}}
\@writefile{toc}{\contentsline {subsection}{\numberline {2.2}Hot Jupiters}{1}}
\@writefile{toc}{\contentsline {subsection}{\numberline {2.3}Water Worlds}{2}}
\@writefile{toc}{\contentsline {subsection}{\numberline {2.4}Exo-Earths}{2}}
\@writefile{toc}{\contentsline {subsection}{\numberline {2.5}Super-Earths}{2}}
\@writefile{toc}{\contentsline {subsection}{\numberline {2.6}Chthonian Planets}{2}}
\@writefile{toc}{\contentsline {section}{\numberline {3}Detection Methods}{2}}
\@writefile{toc}{\contentsline {subsection}{\numberline {3.1}Transit Method/Light Curves}{2}}
\@writefile{lof}{\contentsline {figure}{\numberline {1}{\ignorespaces The diagram of an exoplanet transit. The planet, small, dark circle, crosses in front of the star as seen from Earth. In the process, it blocks out some light. The light curve, shown on the bottom, is a plot of brightness versus time, and shows that the star brightness is steady until the exoplanet starts to cover up some of the visible surface of the star. As it does so, the star dims. It eventually returns back to its normal brightness only to await the next transit.}}{3}}
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\@writefile{toc}{\contentsline {subsection}{\numberline {3.2}Direct Detection}{4}}
\@writefile{lof}{\contentsline {figure}{\numberline {2}{\ignorespaces A coronagraphic image of an exoplanet orbiting the star Fomalhaut (inside the box, with the arrow labeled ``2012''). This image was obtained with the Hubble Space Telescope, and the star's light has been blocked-out using a small metal disk. Fomalhaut is also surrounded by a dusty disk of material---the broad band of light that makes a complete circle around the star. This band of dusty material is about the same size as the Kuiper belt in our solar system. The planet, ``Fomalhaut B'', is estimated to take 1,700 years to orbit once around the star. Thus, using Kepler's third law (P$^{\rm  2}$ $\propto $ a$^{\rm  3}$), it is roughly about 140 AU from Fomalhaut (remember that Pluto orbits at 39.5 AU from the Sun).}}{4}}
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\@writefile{toc}{\contentsline {subsection}{\numberline {3.3}Radial Velocity (Stellar Wobble)}{5}}
\@writefile{toc}{\contentsline {section}{\numberline {4}Characterizing Exoplanets from Transit Light Curves}{5}}
\@writefile{lof}{\contentsline {figure}{\numberline {3}{\ignorespaces An exoplanet transit light curve (bottom) can provide a useful amount of information. The most important attribute is the radius of the exoplanet. But if you know the mass and radius of the exoplanet host star, you can determine other details about the exoplanet's orbit. As the figure suggests, by observing multiple transits of an exoplanet, you can actually determine whether it has a moon! This is because the exoplanet and its moon orbit around the center of mass of the system (``barycenter''), and thus the planet appears to wobble back and forth relative to the host star.}}{6}}
\newlabel{transit}{{3}{6}}
\@writefile{toc}{\contentsline {section}{\numberline {5}Deriving Parameters from Transit Light Curves}{6}}
\@writefile{lof}{\contentsline {figure}{\numberline {4}{\ignorespaces The light curve of Kepler 1b as measured by the {\it  Kepler} satellite. The numbers on the y-axis are the total counts (how much light was measured), while the x-axis is ``modified Julian days''. This is a system that simply makes it easy to figure out periods of astronomical events since it is a number that increases by 1 every day (instead of figuring out how many days there were between June 6$^{\rm  th}$ and November 3$^{\rm  rd}$). Thus, to get an orbital period you just subtract the MJD of one event from the MJD of the next event.}}{7}}
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\@writefile{lof}{\contentsline {figure}{\numberline {5}{\ignorespaces Transiting exoplanet \#1. The vertical line in the center of the plot simply identifies the center of the eclipse.}}{8}}
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\@writefile{lof}{\contentsline {figure}{\numberline {6}{\ignorespaces Transiting exoplanet \#2.}}{8}}
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\@writefile{lof}{\contentsline {figure}{\numberline {7}{\ignorespaces Transiting exoplanet \#3.}}{9}}
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\@writefile{lof}{\contentsline {figure}{\numberline {8}{\ignorespaces Transiting exoplanet \#4.}}{9}}
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\@writefile{lof}{\contentsline {figure}{\numberline {9}{\ignorespaces Transiting exoplanet \#5.}}{10}}
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\@writefile{lof}{\contentsline {figure}{\numberline {10}{\ignorespaces Transiting exoplanet \#6.}}{10}}
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\@writefile{lof}{\contentsline {figure}{\numberline {11}{\ignorespaces Transiting exoplanet \#7.}}{11}}
\newlabel{transit07}{{11}{11}}
\@writefile{lof}{\contentsline {figure}{\numberline {12}{\ignorespaces Transiting exoplanet \#8.}}{11}}
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\@writefile{lot}{\contentsline {table}{\numberline {1}{\ignorespaces Exoplanet Host Star Data}}{12}}
\newlabel{hostdata}{{1}{12}}
\@writefile{lot}{\contentsline {table}{\numberline {2}{\ignorespaces Exoplanet Data}}{13}}
\newlabel{exodata}{{2}{13}}
\@writefile{toc}{\contentsline {section}{\numberline {6}The Habitable Zone}{14}}
\@writefile{toc}{\contentsline {section}{\numberline {7}Classifying Your Exoplanets}{16}}
\@writefile{lot}{\contentsline {table}{\numberline {3}{\ignorespaces Solar System Data}}{17}}
\newlabel{solarsystem}{{3}{17}}
\@writefile{toc}{\contentsline {section}{\numberline {8}Take Home Exercise (35 points total)}{19}}
\@writefile{toc}{\contentsline {subsection}{\numberline {8.1}Possible Quiz Questions}{19}}
\@writefile{toc}{\contentsline {subsection}{\numberline {8.2}Extra Credit (ask your TA for permission before attempting, 5 points )}{19}}