It has been suggested that the haze aerosols in Titan's atmosphere mig
ht present an irregular structure, rather similar to the morphology of
aggregates experimentally synthesized by Bar-Nun et al. (J. geophys.
Res. 93, 8383, 1988). The theoretical approach of West (Appl. Opt. 30,
5316, 1991) and West and Smith (Icarus 90, 330, 1991), which uses a f
ractal concept to numerically generate aggregates, allowed us to suppo
rt this idea and to provide constraints on their size and shape by com
paring the observed and modelled polarization properties of such parti
cles. The building mechanism of these aerosols, when analysed using mi
crophysical modelling (Cabane et al., Icarus %, 176, 1992), leads natu
rally to aggregates. They are formed of spherical compact monomers, wh
ich build up in the region of photochemical synthesis, and whose radiu
s depends mainly on the atmospheric pressure at the formation level. T
he subsequent growth of aggregates in the settling phase is treated he
re by introducing the fractal dimension as a parameter of the model (D
(f) almost-equal-to 2 in the case of cluster-cluster aggregation). Usi
ng this fractal model, a vertical distribution of size and number dens
ity of the aggregates is obtained down to almost-equal-to 80 km for di
fferent production altitudes. The previous estimate of the formation a
ltitude of photochemical aerosols (almost-equal-to 350-400 km) is conf
irmed when comparing the number of monomers per aggregate deduced from
the present study with the value proposed by West and Smith. The vert
ical profile of the effective radius of aggregates is calculated as a
function of the visible optical depth derived from Voyager imaging. A
good fit with the radius derived from Voyager forward-scattering measu
rements is obtained (almost-equal-to 0.3-0.5 mum), still using a low f
ormation altitude. Finally, it must be emphasized that, for the first
time, observational and theoretical results about the size and the str
ucture of particles are reconciled.