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We show that the low-velocity 56Ni decay lines detected earlier than expectedin the type Ia SN 2014J find an explanation in the Quark-Nova Ia model whichinvolves the thermonuclear explosion of a tidally disrupted sub-ChandrasekharWhite Dwarf in a tight Neutron-Star-White-Dwarf binary system. The explosion istriggered by impact from the Quark-Nova ejecta on the WD material; theQuark-Nova is the explosive transition of the Neutron star to a Quark startriggered by accretion from a CO torus (the circularized WD material). Thepresence of a compact remnant (the Quark Star) provides: (i) an additionalenergy source (spin-down power) which allows us to fit the observed light-curveincluding the steep early rise; (ii) a central gravitational potential whichslows down some of the 56Ni produced to velocities of a few 1000 km/s. In ourmodel, the 56Ni decay lines become optically visible at ~20 days from explosiontime in agreement with observations. We list predictions that can provideimportant tests for our model.

The puzzling early detection of low velocity 56Ni decay lines in SN 2014J: Hints of a compact remnant