  We present simulated observations of the Doppler shifts of the solar Mg I
Fraunhofer line scattered by asteroidal, cometary, and trans-Neptunian dust
particles. The studies are based on the results of integrations of orbital
evolution of particles under the gravitational influence of planets, the
Poynting-Robertson drag, radiation pressure, and solar wind drag. The derived
shifts in the centroid and profile of the line with solar elongation are
different for different sources of dust. A comparison of the velocities of
zodiacal dust particles based on these numerical integrations with the
velocities obtained from WHAM observations shows that the fraction of cometary
dust particles among zodiacal dust particles is significant and can be
dominant. A considerable fraction of trans-Neptunian dust particles among
zodiacal dust particles also fits different observations. The mean eccentricity
of zodiacal dust particles is estimated to be about 0.5.
