  Almost all superluminous supernovae (SLSNe) whose peak magnitudes are
$\lesssim -21$ mag can be explained by the $^{56}$Ni-powered model,
magnetar-powered (highly magnetized pulsar) model or ejecta-circumstellar
medium (CSM) interaction model. Recently, iPTF13ehe challenges these
energy-source models, because the spectral analysis shows that $\sim
2.5M_\odot$ of $^{56}$Ni have been synthesized but are inadequate to power the
peak bolometric emission of iPTF13ehe, while the rebrightening of the late-time
light-curve (LC) and the H$\alpha$ emission lines indicate that the ejecta-CSM
interaction must play a key role in powering the late-time LC. Here we propose
a triple-energy-source model, in which a magnetar together with some amount
($\lesssim 2.5M_\odot$) of $^{56}$Ni may power the early LC of iPTF13ehe while
the late-time rebrightening can be quantitatively explained by an ejecta-CSM
interaction. Furthermore, we suggest that iPTF13ehe is a genuine core-collapse
supernova rather than a pulsational pair-instability supernova candidate.
Further studies on similar SLSNe in the future would eventually shed light on
their explosion and energy-source mechanisms.
