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$\begin{figure} \par {\includegraphics[width=8.8cm,clip]{He021fig1.ps} } \end{figure}$ Figure 1: shows the re-scaled Roche lobes (contours of the effective potential) in the equatorial xz plane ( lower half) and in the vertical yz plane ( upper half) of a hypothetical isolated Earth-Sun binary with a mass ratio $3\times 10^{-6}$ in the strong gravity regime (say with the separation $D_{\rm o}=1$ AU, thin blue lines), and in the weak gravity regime (say with separation $D_{\rm o}=0.1$ pc and $GM_\odot D_{\rm o}^{-2}a_0^{-1} \sim 0.1$ , shaded areas). The Earth is at origin and the Sun is at unit length to the right. The inner Lagrangian point is a saddle point between the Earth and the Sun, which is slightly further away from the Earth in the deep-MOND regime than in strong gravity regime.
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In the text

$\begin{figure} \par {\includegraphics[width=8.2cm,clip]{He021fig2.ps} } \end{figure}$ Figure 2: shows the MONDian "filling factor'' for outer Galactic satellites (20-200 kpc), i.e., the ratio of the observed limiting radius $r_{\rm lim}$ and the instantaneous Intermediate Roche radius $r_{\rm IR}$ (cf. Eq. (15), with a nominal luminosity $L_{\rm MW}=4\times 10^{10}~L_\odot$ for the Galaxy). The overall distribution is much broader than the range expected in MOND (indicated between the two thick dashed lines), and many are outliers with $r_{\rm lim}>r_{\rm IR}$ . The symbol sizes are proportional to the apparent limitting sizes ${r_{\rm lim} \over D}$ of satellites (the smallest/biggest symbols correspond to physical radii of 40 pc/4000 pc, observational errors on distance and $\theta _{\rm lim}$ are 10% typically), and the sample includes both globular clusters and dwarf galaxies with luminosities between $10^5{-}10^{6.5}~L_\odot$ (data from Harris 1996; Mateo 1998).
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In the text