The puzzling early detection of low velocity 56Ni decay lines in SN 2014J: Hints of a compact remnant
arXiv:1410.4264 · doi:10.1088/0004-637X/801/1/64
Abstract
We show that the low-velocity 56Ni decay lines detected earlier than expected in the type Ia SN 2014J find an explanation in the Quark-Nova Ia model which involves the thermonuclear explosion of a tidally disrupted sub-Chandrasekhar White Dwarf in a tight Neutron-Star-White-Dwarf binary system. The explosion is triggered by impact from the Quark-Nova ejecta on the WD material; the Quark-Nova is the explosive transition of the Neutron star to a Quark star triggered by accretion from a CO torus (the circularized WD material). The presence of a compact remnant (the Quark Star) provides: (i) an additional energy source (spin-down power) which allows us to fit the observed light-curve including the steep early rise; (ii) a central gravitational potential which slows down some of the 56Ni produced to velocities of a few 1000 km/s. In our model, the 56Ni decay lines become optically visible at ~20 days from explosion time in agreement with observations. We list predictions that can provide important tests for our model.
arXiv comment6 pages, 3 figures and 1 Table. Accepted for publication in ApJ. Details on how we compute the Quark-Nova Ia (QNIa) light-curve are provided (see new Appendix). Relevant codes and usage instructions available via a URL link provided in the Appendix. Comments welcome
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