Using both shell-flash and realistic models on accreting neutron stars with the full nuclear reaction network up to Bi, we investigate the detailed relation between the final products of the rp-process and the ignition pressure. We find that nuclear fuels of H and 4He are almost burned out after the flash and that the mass number of synthesized nuclei reaches to ~=100 in the pressure range from 1023 to 1023.5 dyn cm-2 for a neutron star of 1.4 Msolar and 10 km radius. Furthermore, p-nuclei up to 126Xe are found to be produced after the flash, thanks to our large network. The postprocess nucleosynthesis for accretion rates of 3×10-10, 3×10-9, and 10-8 Msolar yr-1, which corresponds to an ignition pressure from 1022.7 to 1022.9 dyn cm-2, reveals that H is exhausted completely during the burst. This is because H decreases significantly as a result of the steady burning before the burst and convective mixing at the initial stage; we find that 64Zn is the most abundant element after the burst.