\relax 
\@writefile{toc}{\contentsline {chapter}{\numberline {1}Introduction}{1}}
\@writefile{lof}{\addvspace {10\p@ }}
\@writefile{lot}{\addvspace {10\p@ }}
\newlabel{ch:introduction}{{1}{1}}
\@writefile{toc}{\contentsline {section}{\numberline {1.1}The evolution of single stars}{1}}
\newlabel{sec:single_stars}{{1.1}{1}}
\@writefile{toc}{\contentsline {section}{\numberline {1.2}Binary-star evolution}{2}}
\newlabel{sec:binaries}{{1.2}{2}}
\@writefile{lof}{\contentsline {figure}{\numberline {1.1}{\ignorespaces A computer model for the evolution of a star of 1\tmspace  +\thinmuskip {.1667em}$M_\odot $ with wind mass loss, calculated with the evolution code of P. Eggleton {1971MNRAS.151..351E,2002ApJ...575..461E}. {\it  Upper panel} ({\bf  a}): A theoretical Hertzsprung-Russell diagram for the model star. The dashed line is where the helium flash takes place; the evolution code replaces the pre-helium-flash model with a post-helium-flash model. The dotted lines are lines of constant radius. {\it  Lower panel} ({\bf  b}): A Kippenhahn diagram that shows the internal structure of the star as a function of time. Grey areas are convective regions, in hatched areas nuclear burning takes place. The thick lines are from top to bottom the mass of the star and the boundaries of the helium and carbon-oxygen core respectively. Some thin burning regions can hardly been seen because they coincide with these thick lines. Notice the changes in scale of the time axis. The labelled points indicate A: zero-age main sequence, B: terminal-age main sequence, C: first dredge-up, D: helium flash, E: zero-age helium main sequence, F: terminal-age helium main sequence, G: early asymptotic giant branch, and H: point where the hydrogen envelope has been blown away and the star starts contracting.  }}{3}}
\newlabel{fig:intro_evolplot}{{1.1}{3}}
\@writefile{toc}{\contentsline {section}{\numberline {1.3}This thesis}{4}}
\newlabel{sec:this_thesis}{{1.3}{4}}
\@writefile{lot}{\contentsline {table}{\numberline {1.1}{\ignorespaces Luminous X-ray binaries in the galactic globular clusters. The columns list the name of the cluster, the position of the source, the orbital period and three indications for an ultra-short (U) or normal (N) period, based on the optical to X-ray luminosity ratio, the maximum luminosity in bursts and the X-ray spectrum. See the main text for more explanation. Adapted from {vl04}.  }}{5}}
\newlabel{tab:lmxbs_in_gcs}{{1.1}{5}}
\@writefile{toc}{\contentsline {subsection}{\numberline {1.3.1}The formation of luminous X-ray binaries in globular clusters}{5}}
\newlabel{sec:this_thesis_ucbs}{{1.3.1}{5}}
\@writefile{lof}{\contentsline {figure}{\numberline {1.2}{\ignorespaces The maximum acceleration along the line of sight $a_\@mathrm {max}$ as a function of the projected distance from the cluster centre, according to a cluster model for NGC\tmspace  +\thinmuskip {.1667em}6624 (curve) compared to the measured position and acceleration of the 11.4\tmspace  +\thinmuskip {.1667em}min binary (dot with error bars). In more recent observations the binary is closer to the centre {1993ApJ...413L.117K}. Taken from {1993MNRAS.260..686V}.  }}{8}}
\newlabel{fig:intro_acceleration}{{1.2}{8}}
\citation{2004ApJ...616L.139W}
\citation{1996MNRAS.282L..37H}
\@writefile{toc}{\contentsline {subsection}{\numberline {1.3.2}The presumed ultra-compact X-ray binary 2S\tmspace  +\thinmuskip {.1667em}0918--549}{9}}
\newlabel{sec:this_thesis_0918}{{1.3.2}{9}}
\citation{2001ApJ...553..335J}
\citation{2001A&A...378L..17N}
\@writefile{toc}{\contentsline {subsection}{\numberline {1.3.3}The formation of double white dwarfs}{11}}
\newlabel{sec:this_thesis_dwds}{{1.3.3}{11}}
\@writefile{lof}{\contentsline {figure}{\numberline {1.3}{\ignorespaces Observations of WD\tmspace  +\thinmuskip {.1667em}0316+768. {\it  Left panel:} Spectrograms (left-most) and the fit to these data. {\it  Right panel:} Radial velocities measured for both components (symbols) and least-squares fits of sine functions to these points (solid curve). Adapted from {2002MNRAS.332..745M}.  }}{12}}
\newlabel{fig:intro_wd0136obs}{{1.3}{12}}
\@writefile{lof}{\contentsline {figure}{\numberline {1.4}{\ignorespaces Schematic representation of the evolution of an initial binary that leads to the double white dwarf WD\tmspace  +\thinmuskip {.1667em}0136+768 with the observed masses, orbital period and age difference. This scenario corresponds to solution\tmspace  +\thinmuskip {.1667em}22 in Table 6.5, in which the primary ejects its envelope with $\gamma \approx 0.95$ (from panel 2 to 3 in the Figure) and the secondary causes a spiral-in with $\alpha _\@mathrm {ce}\approx 1.00$ (panel 4 to 5). The Figure shows the stars and their Roche lobes with respect to the centre of mass of the binary (dotted vertical line). The numbers are the age since the zero-age main sequence, the two masses and the orbital period. The components of the double white dwarf that is formed in this scenario have an age difference of 299\tmspace  +\thinmuskip {.1667em}Myr; compare the observed age difference of 450\tmspace  +\thinmuskip {.1667em}Myr according to the cooling models. The final panel shows the binary at its current age, according to the cooling age for the youngest white dwarf. The final orbital separation is less than 5\tmspace  +\thinmuskip {.1667em}$R_\odot $ and hardly visible.  }}{14}}
\newlabel{fig:intro_rocheplot}{{1.4}{14}}
\@setckpt{../Chapter_1/chapter1}{
\setcounter{page}{15}
\setcounter{equation}{0}
\setcounter{enumi}{0}
\setcounter{enumii}{0}
\setcounter{enumiii}{0}
\setcounter{enumiv}{0}
\setcounter{footnote}{0}
\setcounter{mpfootnote}{0}
\setcounter{part}{0}
\setcounter{chapter}{1}
\setcounter{section}{3}
\setcounter{subsection}{3}
\setcounter{subsubsection}{0}
\setcounter{paragraph}{0}
\setcounter{subparagraph}{0}
\setcounter{figure}{4}
\setcounter{table}{1}
\setcounter{r@tfl@t}{0}
\setcounter{parentequation}{0}
}
