  Understanding the persistent emission is crucial for studying type I X-ray
bursts, which provide insight into neutron star properties. Although accretion
disc coronae appear to be common in many accreting systems, their fundamental
properties remain insufficiently understood. Recent work suggests that Type I
X-ray bursts from accreting neutron stars provide an opportunity to probe the
characteristics of coronae. Several studies have observed hard X-ray shortages
from the accretion disk during an X-ray burst implying strong coronal cooling
by burst photons. Here, we use the plasma emission code EQPAIR to study the
impact of X-ray bursts on coronae, and how the coronal and burst properties
affect the coronal electron temperatures and emitted spectra. Assuming a
constant accretion rate during the burst, our simulations show that soft
photons can cool coronal electrons by a factor of $\gtrsim 10$ and cause a
reduction of emission in the $30$-$50$ keV band to $\lesssim 1\%$ of the
pre-burst emission. This hard X-ray drop is intensified when the coronal
optical depth and aspect ratio is increased. In contrast, depending on the
properties of the burst and corona, the emission in the $8$-$24$ keV band can
either increase, by a factor of $\gtrsim20$, or decrease, down to $\lesssim
1\%$ of the pre-burst emission. An increasing accretion rate during the X-ray
burst reduces the coronal cooling effects and the electron temperature drop can
be mitigated by $\gtrsim60\%$. These results indicate that changes of the hard
X-ray flux during an X-ray burst probe the geometrical properties of the
corona.
