  On 2014 March 29, an intense solar flare classified as X1.0 occurred in the
active region 12017. Several associated phenomena accompanied this event, among
them a fast-filament eruption, large-scale propagating disturbances in the
corona and the chromosphere including a Moreton wave, and a coronal mass
ejection. This flare was successfully detected in multiwavelength imaging in
H-alpha line by the Flare Monitoring Telescope (FMT) at Ica University, Peru.
We present a detailed study of the Moreton wave associated with the flare in
question. Special attention is paid to the Doppler characteristics inferred
from the FMT wing (H-alpha$\pm0.8$~{\AA}) observations, which are used to
examine the downward/upward motion of the plasma in the chromosphere. Our
findings reveal that the downward motion of the chromospheric material at the
front of the Moreton wave attains a maximum velocity of 4 km/s, whereas the
propagation speed ranges between 640 and 859 km/s. Furthermore, utilizing the
weak shock approximation in conjunction with the velocity amplitude of the
chromospheric motion induced by the Moreton wave, we derive the Mach number of
the incident shock in the corona. We also performed the temperature-emission
measure analysis of the coronal wave based on the Atmospheric Imaging Assembly
(AIA) observations, which allowed us to derive the compression ratio, and to
estimate the Alfv\'en and fast-mode Mach numbers of the order of 1.06-1.28 and
1.05-1.27. Considering these results and the MHD linear theory we discuss the
characteristics of the shock front and the interaction with the chromospheric
plasma.
