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\@writefile{lof}{\contentsline {figure}{\numberline {1}{\ignorespaces Flow patterns on the surface of a spherical star irradiated by a parallel beam, for four values of the Coriolis parameter $\beta $. The horizontal lines in the lower panels indicate the location of the critical boundaries $\qopname  \relax o{cos}\theta = \pm 1/\beta $ that separate Coriolis- and drag-dominated flows.}}{4}}
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\@writefile{lof}{\contentsline {figure}{\numberline {2}{\ignorespaces Mesh structure (left), effective temperature (center) and effective gravity (right) for the O6V+O6V model, plotted as a function of sky coordinates $(x,y)$ for pole-on (top) and equator-on (bottom) vantages.}}{6}}
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\@writefile{lof}{\contentsline {figure}{\numberline {3}{\ignorespaces As in Figure\nobreakspace  {}2\hbox {}, except that the Cartesian components of the velocity are now shown in the sky coordinate system (the $z$ axis is directed out of the page).}}{6}}
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\@writefile{lof}{\contentsline {figure}{\numberline {4}{\ignorespaces Snapshots of the isovelocity contours and He\textsc  {ii}\tmspace  +\thinmuskip {.1667em}4026\tmspace  +\thinmuskip {.1667em}\r A\ line profiles for the O6+O6 model, at four selected orbital phases. Only the lower part of the line profiles is shown, in order to emphasize the depth differences. The dashed lines show the corresponding profiles in the absence of surface flows.}}{7}}
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\bibcite{Arias:2002aa}{{1}{2002}{{{Arias} et~al.}}{{{Arias}, {Morrell}, {Barb{\'a}}, {Bosch}, {Grosso} \& {Corcoran}}}}
\bibcite{Drechsel:1995aa}{{2}{1995}{{{Drechsel} et~al.}}{{{Drechsel}, {Haas}, {Lorenz} \& {Gayler}}}}
\bibcite{Eddington:1926ab}{{3}{1926}{{{Eddington}}}{{{Eddington}}}}
\bibcite{Gayley:1999aa}{{4}{1999}{{{Gayley} et~al.}}{{{Gayley}, {Owocki} \& {Cranmer}}}}
\bibcite{Hendry:1992aa}{{5}{1992}{{{Hendry} \& {Mochnacki}}}{{{Hendry} \& {Mochnacki}}}}
\bibcite{Howarth:1997aa}{{6}{1997}{{{Howarth} et~al.}}{{{Howarth}, {Siebert}, {Hussain} \& {Prinja}}}}
\bibcite{Lanz:2003aa}{{7}{2003}{{{Lanz} \& {Hubeny}}}{{{Lanz} \& {Hubeny}}}}
\@writefile{lof}{\contentsline {figure}{\numberline {5}{\ignorespaces The difference (in continuum units) between the depths of the blue- and redshifted He\textsc  {ii}\tmspace  +\thinmuskip {.1667em}4026\tmspace  +\thinmuskip {.1667em}\r A\ line profiles for the O6+O6 model at quadrature, plotted as a function of braking timescale $t_{\rm  b}$ for various choices of the inclination. The maximum surface flow velocity $v_{\rm  max}$ is also shown.}}{8}}
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\bibcite{Lanz:2007aa}{{8}{2007}{{{Lanz} \& {Hubeny}}}{{{Lanz} \& {Hubeny}}}}
\bibcite{Martins:2005aa}{{9}{2005}{{{Martins} et~al.}}{{{Martins}, {Schaerer} \& {Hillier}}}}
\bibcite{Milne:1926aa}{{10}{1926}{{{Milne}}}{{{Milne}}}}
\bibcite{Palate:2013aa}{{11}{2013}{{{Palate} et~al.}}{{{Palate}, {Rauw}, {Koenigsberger} \& {Moreno}}}}
\bibcite{Phillips:2002aa}{{12}{2002}{{{Phillips} \& {Podsiadlowski}}}{{{Phillips} \& {Podsiadlowski}}}}
\bibcite{Tassoul:2000aa}{{13}{2000}{{{Tassoul}}}{{{Tassoul}}}}
\bibcite{Tsantilas:2006aa}{{14}{2006}{{{Tsantilas} et~al.}}{{{Tsantilas}, {Rovithis-Livaniou} \& {Djurasevic}}}}
\bibcite{Vaz:1985aa}{{15}{1985}{{{Vaz} \& {Nordlund}}}{{{Vaz} \& {Nordlund}}}}
\bibcite{von-Zeipel:1924aa}{{16}{1924}{{{von Zeipel}}}{{{von Zeipel}}}}
\bibcite{Wilson:1990aa}{{17}{1990}{{{Wilson}}}{{{Wilson}}}}
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