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Most of accreting NSs, including both BXPs and LMXBs, are expected to be in a condition of near torque equilibrium, namely, [OMEGA] [approximately equal to] [[omega].sub.K]([R.sub.A]), because their spin up/down time scales due to the accretion torque are estimated to be shorter than their life times.
4, the MF strengths of LMXBs have been estimated in this manner, using their fast spins and high luminosities, although the results are rather uncertain, reflecting uncertainties, e.g., in the numerical factor [zeta] in Eq.
It exhibits three broad peaks; one at [B.sub.d] = [10.sup.7]-[10.sup.9]T covering BXPs and the majority of radio pulsars, another for magnetars at [B.sub.d] = [10.sup.10]-[10.sup.11]T, and the other at [B.sub.d] = [10.sup.4]-[10.sup.5]T for MSPs (and LMXBs).
(70) This was also motivated to explain MSPs and LMXBs: a standard view is that they were born as isolated radio pulsars with [B.sub.d] ~ [10.sup.8] T, became slow rotators by losing [E.sub.rot], and weak-[B.sub.d] objects due to the MF decay, and captured by a low-mass star to become LMXBs, wherein they were spun up ("recycled") by accretion as described by Eq.
The abundance of MSPs and LMXBs can be explained by considering that the dominant NS subclass born with [B.sub.d] = [10.sup.7] - [10.sup.9] T would have mostly completed their transition in ~ [10.sup.9] yr.
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- LN Tolstoi
- LN Tolstoi