  Type I X-ray bursts are rapidly brightening phenomena triggered by
thermonuclear burning on accreting layer of a neutron star (NS). The light
curves represent the physical properties of NSs and the nuclear reactions on
the proton-rich nuclei. The numerical treatments of the accreting NS and
physics of the NS interior are not established, which shows uncertainty in
modelling for observed X-ray light curves. In this study, we investigate
theoretical X-ray-burst models, compared with burst light curves with
GS~1826-24 observations. We focus on the impacts of the NS mass, the NS radius,
and base-heating on the NS surface using the MESA code. We find a monotonic
correlation between the NS mass and the parameters of the light curve. The
higher the mass, the longer the recurrence time and the greater the peak
luminosity. While the larger the radius, the longer the recurrence time, the
peak luminosity remains nearly constant. In the case of increasing base
heating, both the recurrence time and peak luminosity decrease. We also examine
the above results using with a different numerical code, HERES, based on
general relativity and consider the central NS. We find that the burst rate,
burst energy and burst strength are almost same in two X-ray burst codes by
adjusting the base-heat parameter in MESA (the relative errors $\lesssim5\%$),
while the duration time and the rise time are significantly different between
(the relative error is possibly $\sim50\%$). The peak luminosity and the
e-folding time are ragged between two codes for different accretion rates.
