  The solar wind is a structured and complex system, in which the fields vary
strongly over a wide range of spatial and temporal scales. As an example, the
turbulent activity in the wind affects the evolution in the heliosphere of the
integral turbulent scale or correlation length [{\lambda}], usually associated
with the breakpoint in the turbulent-energy spectrum that separates the
inertial range from the injection range. This large variability of the fields
demands a statistical description of the solar wind. In this work, we study the
probability distribution function (PDF) of the magnetic autocorrelation lengths
observed in the solar wind at different distances from the Sun. We use
observations from Helios, ACE, and Ulysses spacecraft. We distinguish between
the usual solar wind and one of its transient components (Interplanetary
Coronal Mass Ejections, ICMEs), and study also solar wind samples with low and
high proton beta [\beta_p ]. We find that in the last 3 regimes the PDF of
{\lambda} is a log-normal function, consistent with the multiplicative and
non-linear processes that take place in the solar wind, the initial {\lambda}
(before the Alfv\'enic point) being larger in ICMEs.
