  Freely-propagating global waves in the solar atmosphere are commonly observed
using Extreme UltraViolet passbands (EUV or "EIT waves"), and less regularly in
H-alpha (Moreton-Ramsey waves). Despite decades of research, joint observations
of EUV and Moreton-Ramsey waves remain rare, complicating efforts to quantify
the connection between these phenomena. We present observations of four
homologous global waves originating from the same active region between 28-30
March 2014 and observed using both EUV and H-alpha data. Each global EUV wave
was observed by the Solar Dynamics Observatory, with the associated
Moreton-Ramsey waves identified using the Global Oscillations Network Group
(GONG) network. All of the global waves exhibit high initial velocity (e.g.,
842-1388 km s$^{-1}$ in the 193A passband) and strong deceleration (e.g., -1437
- -782 m s$^{-2}$ in the 193A passband) in each of the EUV passbands studied,
with the EUV wave kinematics exceeding those of the Moreton-Ramsey wave. The
density compression ratio of each global wave was estimated using both
differential emission measure and intensity variation techniques, with both
indicating that the observed waves were weakly shocked with a fast magnetosonic
Mach number slightly greater than one. This suggests that, according to current
models, the global coronal waves were not strong enough to produce
Moreton-Ramsey waves, indicating an alternative explanation for these
observations. Instead, we conclude that the evolution of the global waves was
restricted by the surrounding coronal magnetic field, in each case producing a
downward-angled wavefront propagating towards the north solar pole which
perturbed the chromosphere and was observed as a Moreton-Ramsey wave.
