  Recent observations in extreme-ultraviolet (EUV) wavelengths reveal an EUV
late phase in some solar flares that is characterized by a second peak in warm
coronal emissions ($\sim3$~MK) several tens of minutes to a few hours after the
soft X-ray (SXR) peak. Using the model enthalpy-based thermal evolution of
loops (EBTEL), in this paper we numerically probe the production of EUV
late-phase solar flares. Starting from two main mechanisms of producing the EUV
late phase, i.e., long-lasting cooling and secondary heating, we carry out two
groups of numerical experiments to study the effects of these two processes on
the emission characteristics in late-phase loops. In either of the two
processes an EUV late-phase solar flare that conforms to the observational
criteria can be numerically synthesized. However, the underlying hydrodynamic
and thermodynamic evolutions in late-phase loops are different between the two
synthetic flare cases. The late-phase peak due to a long-lasting cooling
process always occurs during the radiative cooling phase, while that powered by
a secondary heating is more likely to take place in the conductive cooling
phase. We then propose a new method for diagnosing the two mechanisms based on
the shape of EUV late-phase light curves. Moreover, from the partition of
energy input, we discuss why most solar flares are not EUV late flares.
Finally, by addressing some other factors that may potentially affect the loop
emissions, we also discuss why the EUV late phase is mainly observed in warm
coronal emissions.
