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Type-Ia supernovae result from binary systems that include a carbon-oxygenwhite dwarf, and these thermonuclear explosions typically produce 0.5 M_solarof radioactive 56Ni. The 56Ni is commonly believed to be buried deeply in theexpanding supernova cloud. Surprisingly, in SN2014J we detected the lines at158 and 812 keV from 56Ni decay ({\tau}~8.8 days) earlier than the expectedseveral-week time scale, only ~20 days after the explosion, and with fluxlevels corresponding to roughly 10% of the total expected amount of 56Ni. Somemechanism must break the spherical symmetry of the supernova, and at the sametime create a major amount of 56Ni at the outskirts. A plausible explanation isthat a belt of helium from the companion star is accreted by the white dwarf,where this material explodes and then triggers the supernova event.

Early 56Ni decay {\gamma}-rays from SN2014J suggest an unusual explosion