We investigate the “antiglitch” AXP 1E 2259+586 experienced between MJD=56031 and 56045 in the context of the Quark-Nova model in which an AXP is a quark star surrounded by a degenerate Keplerian disk. In a companion paper we assumed the “anti-glitch” to be instantaneous, whereas in this paper we consider the quark star to undergo a period of enhanced spin-down over several days. We find that the Quark-Nova model can account for the spin-down and at the same time the enhanced 2–10 keV observed flux without introducing any new physics to the model.
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In our companion paper (Ouyed et al. 2013) we consider a retrograde ring. In this case the angular momentum transfer will spin down the QS during step 2 above instead of spinning it up. The rest of the steps will proceed as normal, including the removal of the atmosphere and enhanced spin down rate.
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This work is funded by the Natural Sciences and Engineering Research Council of Canada. N. Koning would like to acknowledge support from the Killam Trusts.
Appendix: Mass loss due to wind
Appendix: Mass loss due to wind
The mass loss from the ring atmosphere is given by equation B.6 in Ouyed et al. (2007b):
where R in,25 is the inner radius of the ring in units of 25 km, T ring,keV is the temperature of the ring in units of keV, and M QS,1.5 is the mass of the QS in units of 1.5 M⊙. The mean molecular weight of the atmosphere, μ atm(t), evolves in time after a burst according to equation 27 in Ouyed et al. (2007b):
where μ q and μ b are the mean molecular weight of the atmosphere in quiescence and during the burst respectively. τ is given by equation 26 in Ouyed et al. (2007b):
where η 0.1 is the wall accretion efficiency in unis of 0.1. If we assume a fraction of the mass-loss, β, is removed as the wind then (1−β) is available for accretion onto the QS giving an accretion luminosity of:
Equation B.13 in Ouyed et al. (2007b) then gives the equilibrium temperature of the ring:
The total mass lost due to the wind from the time of the burst, t b , to time t is:
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Koning, N., Leahy, D. & Ouyed, R. “Anti-glitches” in the Quark-Nova model for AXPs II. Astrophys Space Sci 350, 701–705 (2014). https://doi.org/10.1007/s10509-014-1787-0
- Stars: neutron
- Stars: individual (1E 2259+586)
- X-Rays: bursts