  Gravitational-wave observatories become more sensitive with each observing
run, increasing the number of detected gravitational-wave signals. A limiting
factor in identifying these signals is the presence of transient non-Gaussian
noise, which generates glitches that can mimic gravitational wave signals. Our
work provides a quasi-physical model waveform for the four most common types of
short transient glitches, which are particularly problematic in the search for
high-mass black hole binaries. Our model has only a few, physically
interpretable parameters: central frequency, bandwidth, phase, amplitude and
time. We demonstrate the accuracy of this model by fitting and removing a large
sample of glitches from a month of LIGO and Virgo data from the O3 observing
run. We can effectively remove three of the four types of short transients. We
finally map the ability of these glitches to mimic binary black hole signals.
