Simulation of shell structures of comet Hale–Bopp

We present a simulation based on the morphology of inner coma of comet Hale–Bopp(C/1995 O1) which was observed in Shanghai Astronomical Observatory using a 1.56 m telescope in February 1997. The simulation is based on spin stable. Two active regions are suggested by the coma morphology. The dust grains are ejected from the rotating nucleus and subjected to the solar radiation pressure. The trajectories are projected on the sky plane and then they are compared to the observational data. The synthetic images can fit the observation images well. Extended active regions are induced to simulate coma morphology. The results show the spin mode may be a simple one. The precession component, if it exists, may be very small. The RA and Dec. of the pole position of comet Hale–Bopp is 250° and −60° (2000 epoch). Two active sources, latitude of 4° and 34° were simulated according to the morphology.