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\@writefile{toc}{\contentsline {section}{\numberline {1}\bf  Discovering Exoplanets}{1}}
\@writefile{toc}{\contentsline {subsection}{\numberline {1.1}Introduction}{1}}
\@writefile{toc}{\contentsline {section}{\numberline {2}Why are Exoplanets so hard to see?}{2}}
\@writefile{lof}{\contentsline {figure}{\numberline {1}{\ignorespaces Comparison of the size of the Earth and Jupiter to the Sun.}}{2}}
\newlabel{suncomp}{{1}{2}}
\@writefile{toc}{\contentsline {section}{\numberline {3}Exoplanet Transits}{3}}
\@writefile{lof}{\contentsline {figure}{\numberline {2}{\ignorespaces A planet 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}}
\newlabel{exoimage}{{2}{4}}
\@writefile{lof}{\contentsline {figure}{\numberline {3}{\ignorespaces The diagram of an exoplanet transit. The planet, small, dark circle/ disk, 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, a plot of brightness versus time, 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.}}{4}}
\newlabel{transit}{{3}{4}}
\@writefile{lot}{\contentsline {table}{\numberline {1}{\ignorespaces Exoplanet Transit Data}}{6}}
\newlabel{measurement}{{1}{6}}
\@writefile{lof}{\contentsline {figure}{\numberline {4}{\ignorespaces The light curve of the transit of the small planet.}}{6}}
\newlabel{smalltransit}{{4}{6}}
\@writefile{lof}{\contentsline {figure}{\numberline {5}{\ignorespaces The light curve of the transit of the large planet.}}{7}}
\newlabel{bigtransit}{{5}{7}}
\@writefile{toc}{\contentsline {subsection}{\numberline {3.1}Real exoplanet transits}{7}}
\@writefile{lof}{\contentsline {figure}{\numberline {6}{\ignorespaces An exoplanet transit light curve (bottom) can provide a useful amount of information. As we have shown, 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. We will discuss center of mass, and the orbits of stars and exoplanets around the center of mass, in the next section.}}{9}}
\newlabel{bigexoplanet}{{6}{9}}
\@writefile{toc}{\contentsline {section}{\numberline {4}Exoplanet Detection by Radial Velocity Variations}{10}}
\@writefile{lof}{\contentsline {figure}{\numberline {7}{\ignorespaces Center of mass, ``x$_{\rm  CM}$'', for two objects that have unequal masses. The center of mass can be thought as being the point where the system would balance on a ``fulcrum'' if connected by a rod.}}{10}}
\newlabel{com}{{7}{10}}
\@writefile{lof}{\contentsline {figure}{\numberline {8}{\ignorespaces If two stars are orbiting around each other, or a planet is orbiting a star, they both {\it  actually} orbit the center of mass. If the two objects have the same mass, the center of mass is exactly halfway between the two objects. Otherwise, the orbits have different sizes.}}{12}}
\newlabel{com2}{{8}{12}}
\@writefile{toc}{\contentsline {section}{\numberline {5}Radial Velocity and the Doppler Effect}{17}}
\@writefile{lof}{\contentsline {figure}{\numberline {9}{\ignorespaces For a stationary vehicle emitting sound, there is no Doppler effect. As the vehicle begins to move, however, the sound is compressed in the direction it is moving, and stretched-out in the opposite direction.}}{17}}
\newlabel{doppler}{{9}{17}}
\@writefile{lof}{\contentsline {figure}{\numberline {10}{\ignorespaces A radial velocity curve (left) for a planet with a one year orbit like Earth, but that imparts a reflex velocity of 1.5 km/hr on its host star. When the motion is directly away from us, \#2, we have the maximum amount of positive radial velocity. When the motion of the object is directly towards us, \#4, we have the maximum negative radial velocity. At points \#1 and \#3, the object is not coming towards us, or going away from us, thus its radial velocity is 0 km/hr. The orbit of the object around the center of mass (``X'') is shown in the right hand panel, where the observer is at the bottom of the diagram. The numbered points represent the same places in the orbit in both panels.}}{18}}
\newlabel{radvel}{{10}{18}}
\@writefile{toc}{\contentsline {subsection}{\numberline {5.1}Take-Home Exercise (35 points total)}{20}}
\@writefile{toc}{\contentsline {subsection}{\numberline {5.2}Possible Quiz Questions}{21}}
\@writefile{toc}{\contentsline {subsection}{\numberline {5.3}Extra Credit (make sure you get permission from your TA before attempting, 5 points)}{21}}