  We present a new non-convex model of the binary asteroid (809) Lundia. A SAGE
(Shaping Asteroids with Genetic Evolution) method using disc-integrated
photometry only was used for deriving physical parameters of this binary
system. The model of (809) Lundia improves former system's pole solution and
gives the ecliptic coordinates of the orbit pole - $\lambda=122^{\circ}$,
$\beta=22^{\circ}$, $\sigma=\pm5^{\circ}$ - and the orbital period of $15.41574
\pm 0.00001$ h. For scaling our results we used effective diameter of $D_{eff}
= 9.6 \pm 1.1$ km obtained from Spitzer observations. The non-convex shape
description of the components permitted a refined calculation of the
components' volumes, leading to a density estimation of $2.5\pm0.2$ g/cm$^3$
and macroporosity of 13-23\%. The intermediate-scale features of the model may
also offer new clues on the components' origin and evolution.
