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\@writefile{toc}{\contentsline {chapter}{\numberline {1}The Dynamics of Supermassive Black Holes in a Gaseous Medium}{1}}
\@writefile{toc}{\contentsline {section}{\numberline {1.1}Problem Setup}{1}}
\@writefile{toc}{\contentsline {section}{\numberline {1.2}Comparison to the Stellar Case}{1}}
\newlabel{fig1}{{1.2}{2}}
\@writefile{lof}{\contentsline {figure}{\numberline {1.1}{\ignorespaces The plot shows the evolution of the distance (in code units) of the SMBH measured from the center of mass of the isothermal sphere. The lines are the results for: gaseous sphere (red), stellar sphere (black) and Chandrasekhar's dynamical friction formula (green).}}{2}}
\@writefile{toc}{\contentsline {section}{\numberline {1.3}Evolution of a binary SMBH}{2}}
\bibcite{}{1}
\newlabel{fig2}{{1.2}{3}}
\@writefile{lof}{\contentsline {figure}{\numberline {1.2}{\ignorespaces The plot shows the evolution of the distance (in code units) of the SMBH measured from the center of mass of the adiabatic sphere. The lines are the predictions for: gaseous sphere (red), stellar sphere (black). The velocity of the SMBH became subsonic at t=9 for gas \& t=15 for the stellar case.}}{3}}
\@writefile{toc}{\contentsline {section}{\numberline {1.4}Conclusions}{3}}
\bibcite{}{2}
\bibcite{}{3}
\bibcite{}{4}
\newlabel{fig3}{{1.3}{4}}
\@writefile{lof}{\contentsline {figure}{\numberline {1.3}{\ignorespaces The plot (top) shows the evolution of the binary in the isothermal sphere, the different curves represents the separation between the black holes for different mass ratios: $M_{binary}=0.02M_{gas}$ (red), $M_{binary} = 0.06M_{gas}$ (blue), $M_{binary} = 0.1M_{gas}$ (green). The bottom figure presents the same evolution but in an adiabatic sphere. }}{4}}
\@writefile{toc}{\contentsline {schapter}{{\normalfont  \rmfamily  References}}{4}}
\newlabel{fig4}{{1.3}{5}}
\@writefile{lof}{\contentsline {figure}{\numberline {1.4}{\ignorespaces Top: The colors in the figure represent the density enhancement $(\rho (t)/\rho (0))$ in the isothermal sphere at the plane of the orbit (z=0) for t=1. The arrows are the two dimensional velocity field of the gas. The white and red curves are the individual orbits of the SMBH's between t=0 and t=1. In this simulation the mass of the binary is 2\% of the mass of the gas. bottom: Same as above in the adiabatic sphere.}}{5}}