  The simulated Doppler shifts of the solar Mg I Fraunhofer line produced by
scattering on the solar light by asteroidal, cometary, and trans-Neptunian dust
particles are compared with the shifts obtained by Wisconsin H-Alpha Mapper
(WHAM) spectrometer. The simulated spectra are based on the results of
integrations of the orbital evolution of particles. The deviation of the
derived spectral parameters for various sources of dust used in the model
reached maximum at the elongation (measured eastward from the Sun) between 90
deg and 120 deg. For the future zodiacal light Doppler shifts measurements, it
is important to pay a particular attention to observing at this elongation
range. At the elongations of the fields observed by WHAM, the model-predicted
Doppler shifts were close to each other for several scattering functions
considered. Therefore the main conclusions of our paper don't depend on a
scattering function and mass distribution of particles if they are reasonable.
A comparison of the dependencies of the Doppler shifts on solar elongation and
the mean width of the Mg I line modeled for different sources of dust with
those obtained from the WHAM observations shows that the fraction of cometary
particles in zodiacal dust is significant and can be dominant. Cometary
particles originating inside Jupiter's orbit and particles originating beyond
Jupiter's orbit (including trans-Neptunian dust particles) can contribute to
zodiacal dust about 1/3 each, with a possible deviation from 1/3 up to 0.1-0.2.
The fraction of asteroidal dust is estimated to be about 0.3-0.5. The mean
eccentricities of zodiacal particles located at 1-2 AU from the Sun that better
fit the WHAM observations are between 0.2 and 0.5, with a more probable value
of about 0.3.
