  We show that a Quark-Nova (QN; the explosive transition of a neutron star to
a quark star) occurring a few days following the supernova explosion of an
Oxygen-type Wolf-Rayet (WO) star can account for the intriguing features of
ASASSN-15lh, including its extreme energetics, its double-peaked light-curve
and the evolution of its photospheric radius and temperature. A two-component
configuration of the homologously expanding WO remnant (an extended envelope
and a compact core) is used to harness the kinetic energy (>10^52 ergs) of the
QN ejecta. The delay between the WO SN and the QN yields a large (~ 10^4 Rsun)
envelope which when energized by the QN ejecta/shock gives the first peak in
our model. As the envelope's photosphere recedes into the slowly expanding, hot
and insulated, denser core (initially heated by the QN shock) a second hump
emerges. The spectrum in our model should reflect the composition of an WO SN
remnant re-heated by a QN going off in its wake.
