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