Abstract
Context. Large all-sky surveys provide us with a lot of photometric data that are sparse in time ( typically a few measurements per night) and can be potentially used for the determination of shapes and rotational states of asteroids.
The method generally used to derive these parameters is the light curve inversion. However, for most asteroids their sparse data are not accurate enough to derive a unique model and the light curve inversion method is thus not very efficient.
Aims. To fully utilize photometry sparse in time, we developed a new simplified model and applied it on the data from the Lowell photometric database.
Our aim was to derive spin axis orientations and shape elongations of asteroids and to find out if there are some differences in distributions of these parameters for selected subpopulations. Methods.
We modeled asteroids as geometrically scattering triaxial ellipsoids. Observed values of mean brightness and the dispersion of brightness were compared with computed values obtained from the parameters of the model, i.e., the ecliptical longitude lambda and latitude beta of the pole and the ratios a/b, b/c of axes of the ellipsoid.
These parameters were optimized to get the best agreement with the observation. Results.
We found that the distribution of lambda for main-belt asteroids is not uniform and is dependent on the inclination of the orbit. Surprisingly, the nonuniformity of lambda distribution is larger for asteroids residing on low-inclination orbits.
We also studied distributions of a/b for several groups of asteroids and found that small asteroids (D < 25 km) are on average more elongated than large ones.