Computer Science
Scientific paper
Sep 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001esasp.459..169z&link_type=abstract
In: Exploring the gamma-ray universe. Proceedings of the Fourth INTEGRAL Workshop, 4-8 September 2000, Alicante, Spain. Editor:
Computer Science
1
Magnetars, X-Ray Binaries, X-Ray Pulsars
Scientific paper
Magnetic fields of accreting X-ray pulsars, estimated from the assumption of their equilibrium rotation are compared with the estimates based on the cyclotron lines observed in their spectra. The comparison indicates that equilibrium rotation assumption is probably correct for pulars fed by Roche lobe overflows and by slow equatorial winds of Be stars. It is definitely not correct for pulsars fed by fast winds. Analysis of all kinds of available information about magnetic fields of accreting X-ray pulsars does not support the existence of magnetars among them. In fact, this should not be surprising, because, due to very short lifetime of a magnetar (104 - 105 yr), the chance of observing it as an accreting object is very small. However, there should be many former magnetars in the binary systems. Some of them might be identifiable through backtracking their spin evolution. The system 2S 0114+650 (Li and van den Heuvel, 1999) remains, so far, as the only strong candidate. However, it would be interesting to measure (with the help of the cyclotron lines) the magnetic fields of the four very slow (Ps ~ 405 - 1413 s) rotators accreting from Be stars, to check, if they also rotate at equilibrium periods. If they do, then one of them (RX J0146.9+6121) might be not a former but just a present day magnetar.
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