1 Introduction

Ground-based modelling of the shape and the rotation of the minor planets requires high precision and long-term photometric observations. With the advent of the CCD era it has become possible to study much fainter minor planets than previously. The photometric methods of modelling are based on multi-opposition lightcurves of full phase coverage obtained at very different longitudes (De Angelis 1993; Detal et al. 1994; Szabó et al. 1999). aspect is to detect possible collisional effects, e.g. multiperiodic lightcurves due to binarity or precession, as they may yield insights into the recent solar system evolution.

We started a long-term observational project addressed to photometric monitoring of selected minor planets. The observing programme consists of asteroids with available multi-opposition lightcurves enabling application of different photometric methods in order to model their shape and rotation. First results of this project have already been published in Sárneczky et al. (1999) and Szabó et al. (1999). The main aim of this paper is to present new CCD observations carried out between October, 1998 and January, 1999 and models for 3 minor planets. Observations, their limitations and applied methods are discussed in Sect. 2, while Sect. 3 deals with the detailed observational results.