Anomalous X-ray Pulsars

Details Anomalous X-ray Pulsars Anomalous X-ray Pulsars

Oct 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000head....5.3601v&link_type=abstract

American Astronomical Society, HEAD Meeting #5, #36.01; Bulletin of the American Astronomical Society, Vol. 32, p.1247

Astronomy and Astrophysics

Astronomy

1

Scientific paper

The Anomalous X-ray pulsars are so-called because it is not understood what powers them. Unlike the binary X-ray pulsars, there is no sign of a companion from which matter could be accreted; unlike radio pulsars, the rotational energy loss is insufficient. A number of exotic models have been suggested: accretion in ultra-compact binaries, accretion from an isolated disk left over from the birth process, decay of a super-strong (1015 G) magnetic field in a ``magnetar,'' and spin-down of a rapidly rotating, very massive white dwarf produced in a merger. I will discuss these models, in particular in relation to the recent observational progress that has been made, using precise X-ray timing and deep optical observations.

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