= Solution
A <luminosity> does not determine a stellar <mass> without a <Mass-luminosity relation>[mass-luminosity] <calibration (differential geometry)>[calibration]. Using the usual approximate <Main sequence>[main-sequence] law $L/L_\odot=(M_s/M_\odot)^\alpha$ gives $M_s=3^{1/\alpha}M_\odot$. With $\alpha=3.5$, the numerical results are
$$
\boxed{M_s\simeq1.37M_\odot,\quad M_p\simeq0.39M_J,\quad a\simeq0.101\ \mathrm{AU},\quad \vartheta\simeq2.46\times10^{-4}\ \mathrm{arcsec}.}
$$
The angular <radius> follows directly from $a(\mathrm{AU})/d(\mathrm{pc})$. Taking $\alpha=4$ changes these estimates by only a few percent, but the <calibration (differential geometry)>[calibration] must be stated. Hubble's 2.4 m aperture has visible-light diffraction scale $1.22\lambda/D\simeq0.05$ arcsec at 500 nm, hundreds of times larger. The separation is therefore unresolved even before the severe star/planet contrast is considered.
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