  The aim of this study is to estimate the rotational characteristics of
meteoroids after their release from a comet during normal activity. The results
can serve as initial conditions for further analyses of subsequent evolution of
rotation in the interplanetary space. A sophisticated numerical model was
applied to meteoroids ejected from 2P/Encke comet. The meteoroid shapes were
approximated by polyhedrons with several thousands of surface elements, which
have been determined by 3D laser scanning method of 36 terrestrial rock
samples. These samples came from three distinct sets with different origin and
shape characteristics. Two types of gas-meteoroid interactions (diffuse and
specular reflection of gas molecules from the surface of meteoroid) and three
gas ejection models (leading to very different ejection velocities) were
assumed. The rotational characteristics of ejected meteoroid population were
obtained by numerical integration of equations of motion with random initial
conditions and random shape selection. It was proved, that the results do not
depend on specific set of shape models and that they are applicable to
(unknown) shapes of real meteoroids. A simple relationship between median of
meteoroid spin frequencies $\bar{f}$ (Hz), ejection velocities $v_{\rm ej}$ (m
s$^{-1}$) and sizes $D$ (m) was determined. For diffuse reflection of gas
molecules from meteoroid's surface it is: $\bar{f}\simeq 2\times 10^{-3} v_{\rm
ej} D^{-0.88}$, and for specular reflection of gas molecules from meteoroid's
surface it is: $\bar{f}\simeq 5\times 10^{-3} v_{\rm ej} D^{-0.88}$. The
distribution of spin frequencies is relatively wide; $2\sigma$-interval can be
described as $\sim(0.1, 10)\times \bar{f}$. The results were determined for
2P/Encke comet, but it was shown that their validity is general.
