Astronomy and Astrophysics – Astrophysics – High Energy Astrophysical Phenomena
Scientific paper
2011-11-13
Astronomy and Astrophysics
Astrophysics
High Energy Astrophysical Phenomena
4 journal pages, 1 figure
Scientific paper
We show that appealing to a Quark-Nova in a tight NS-WD binary system, a Type Ia explosion can occur for a narrow range in white dwarf mass (0.5 < M_WD/M_sun < 0.8). These CO WDs are heated by the strong QN shock triggering Carbon burning under degenerate conditions (a QN-Ia). The explosion in our model produces on average half the Nickel yield expected from Chandrasekhar-mass counterparts. We find that Intermediate-Mass X-ray binaries (IMXBs) with donor stars in the 3.5 < M_don./M_sun < 5 range are best candidates for QNe-Ia progenitors. Specifically, IMXBs which evade the common envelope phase and experience an extended accretion phase (preferably with the help of a circumbinary disk), lead to optimum conditions for QNe-Ia. QNe-Ia are naturally linked to star formation (with delays < 10^9 years). If the peak in star formation rate occurred at 1 < z < 2 as observations seem to suggest, QN-Ia rate would peak at 0.75 < z < 1.5, lurking among standard Type Ias. We estimate that a small fraction of IMXBs experiencing a QN-Ia event is enough to make them statistically significant at 0.75 < z < 1.5 in which case, their dimness (by ~ 0.7 magnitudes as compared to their Chandrasekhar-mass counterparts) would have consequences to Cosmology. In today's universe (z<0.75), and z>2 universe, we expect QNe-Ia to manifest themselves as rare sub-Chandrasekhar Type Ias; most likely in star-forming galaxies.
Ouyed Rachid
Staff Jan E.
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