All Figures

$\begin{figure} \par\includegraphics[width=8cm,clip]{fig1.eps} \end{figure}$ Figure 1: Variation of minimum depths of IU Aur with time between 1964 and 2002. Best linear fits (solid lines) are shown. The filled symbols are the result of this work. The figure was adopted from DHLM and complemented by our new data and HIPPARCOS measurements.
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{4221f2.eps}\end{figure}$ Figure 2: 3-D aspect of the IU Aur binary components at first quadrature. The cooler secondary essentially fills its critical Roche lobe.
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In the text

$\begin{figure} \par\includegraphics[width=13.4cm,clip]{4221f3.eps} \end{figure}$ Figure 3: Observed normalized UBVlight curves obtained in 1997/98 (dots) and best fit theoretical curves (solid lines) of IU Aur. The curves are given in intensity units, while B and V data are offset by 0.1 each. Phases were calculated according to the ephemeris of Eq. (1).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{4221f4.eps}\end{figure}$ Figure 4: Upper part: The observed ${\rm O{-}C}_{\rm lin}$ versus phase of the long orbit; $C_{\rm lin}= 2438448.40705+1.8114742.E$ . The full line represents the dynamical term, dot-dashed line is valid for $\omega ^0=24 \hbox {$^\circ $ }$ , dashed line for $\omega ^0=-16\hbox {$^\circ $ }$ . Lower part: Residuals relative to minimum times calculated using the sum of geometrical and dynamical terms.
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In the text

$\begin{figure} \par\includegraphics[width=6.9cm,clip]{fig5.eps}\end{figure}$ Figure 5: Behavior of inclinations. 1: i₁⁰, 2: i₂⁰; long-dashed lines represent limits for mutual eclipses, when i₂⁰ = 88 or $92\hbox {$^\circ $ }$ .
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{fig1.eps} \end{figure}$	Figure 1: Variation of minimum depths of IU Aur with time between 1964 and 2002. Best linear fits (solid lines) are shown. The filled symbols are the result of this work. The figure was adopted from DHLM and complemented by our new data and HIPPARCOS measurements.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{4221f2.eps}\end{figure}$	Figure 2: 3-D aspect of the IU Aur binary components at first quadrature. The cooler secondary essentially fills its critical Roche lobe.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=13.4cm,clip]{4221f3.eps} \end{figure}$	Figure 3: Observed normalized UBVlight curves obtained in 1997/98 (dots) and best fit theoretical curves (solid lines) of IU Aur. The curves are given in intensity units, while B and V data are offset by 0.1 each. Phases were calculated according to the ephemeris of Eq. (1).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=6.9cm,clip]{fig5.eps}\end{figure}$	Figure 5: Behavior of inclinations. 1: i₁⁰, 2: i₂⁰; long-dashed lines represent limits for mutual eclipses, when i₂⁰ = 88 or $92\hbox {$^\circ $ }$ .
Open with DEXTER