\relax 
\@writefile{toc}{\contentsline {subsection}{\numberline {17.3}Stable and Unstable orbits around a Schwarzchild black hole}{119}}
\@writefile{lof}{\contentsline {figure}{\numberline {3}{\ignorespaces The Newtonian effective potential showing how an angular momentum barrier prevents particles reaching $r=0$.}}{119}}
\@writefile{lof}{\contentsline {figure}{\numberline {4}{\ignorespaces The effective potential (4) plotted for several values of the angular momentum parameter $h^\prime $.}}{121}}
\@writefile{toc}{\contentsline {subsection}{\numberline {17.4}Supermassive black holes}{121}}
\@writefile{lof}{\contentsline {figure}{\numberline {5}{\ignorespaces The masing $H_20$ disc in the centre of NGC4258.}}{123}}
\@writefile{lof}{\contentsline {figure}{\numberline {6}{\ignorespaces  The line profile of iron K-alpha from MCG-6-30-15 observed by the ASCA satellite (Tanaka et al, 1995, Nature, 375, 659). The emission line is extremely broad, with a width indicating velocities of order one-third of the speed of light. There is a marked asymmetry towards energies lower than the rest-energy of the emission line (6.4 keV). This asymmetry is most likely caused by gravitational and relativistic-Doppler shifts near the black hole at the center of the galaxy. The solid line shows the model profile expected from a disk of matter orbiting the hole, extending between 3 and 10 Schwarzschild radii.}}{124}}