  Using the MESA code, we have carried out a detailed survey of the available
parameter space for the double-peaked type I X-ray bursts. We find that the
double-peaked structure appears at mass accretion rate $\dot{M}$ in the range
of $\sim(4-8)\times10^{-10}\,M_{\odot}/{\rm yr}$ when metallicity $Z=0.01$,
while in the range of $\sim(4-8)\times10^{-9}\,M_{\odot}/\rm{yr}$ when
$Z=0.05$. Calculations of the metallicity impact suggest that the double peaks
will disappear when $Z\lesssim0.005$ for
$\dot{M}=5\times10^{-10}\,M_{\odot}/\rm{yr}$ and $Z\lesssim0.04$ for
$\dot{M}=5\times10^{-9}\,M_{\odot}/\rm{yr}$. Besides, the impacts of base
heating $Q_{\rm b}$, as well as nuclear reaction waiting points:
$^{22}\rm{Mg}$, $^{26}\rm{Si}$, $^{30}\rm{S}$, $^{34}\rm{Ar}$, $^{56}{\rm Ni}$,
$^{60}\rm Zn$, $^{64}\rm{Ge}$, $^{68}\rm{Se}$, $^{72}\rm{Kr}$ have been
explored. The luminosity of the two peaks decreases as $Q_{\rm b}$ increases.
$^{68}{\rm Se}(p,\gamma){^{69}{\rm Br}}$ is the most sensitive reaction, the
double peaks disappear assuming that $^{56}{\rm Ni}(p,\gamma)^{57}{\rm Cu}$ and
$^{64}{\rm Ge}(p,\gamma)^{65}{\rm As}$ reaction rates have been underestimated
by a factor of 100 and the $^{22}{\rm Mg}(\alpha,p)^{25}{\rm Al}$ reaction rate
has been overestimated by a factor of 100, which indicates that $^{22}{\rm
Mg}$, $^{56}{\rm Ni}$, $^{64}{\rm Ge}$, $^{68}{\rm Se}$ are possibly the most
important nuclear waiting points impedance. Comparisons to the double-peaked
bursts from 4U 1636-53 and 4U 1730-22 suggest that the nuclear origins of
double-peaked type I X-ray bursts are difficult to explain the observed larger
peak times ($t_{\rm p,1}\gtrsim4\,{\rm s}$, $t_{\rm p,2}\gtrsim8\,{\rm s}$) and
smaller peak ratio($r_{1,2}\lesssim0.5$). The composition of ashes from
double-peaked bursts is very different from the single-peaked bursts especially
for the heavier p-nuclei.
