Anomalous X-ray pulsars (AXPs) are now widely believed to be magnetars—young, isolated, highly magnetized neutron stars. These energetic X-ray pulsars are characterized by slow rotation periods of ~2–12 seconds and large magnetic fields of ~1013–1015 gauss (1 to 100 gigateslas). There are currently (as of 2017) 12 confirmed and 2 candidate AXPs.[1] The identification of AXPs with magnetars was motivated by their similarity to another enigmatic class of sources, the soft gamma repeaters.
A list of AXP candidates and their estimated rotation period in seconds, as of 2003, follows:
AXP 1E 2259+586 6.98
AXP 1E 1048-59 6.45
AXP 4U 0142+61 8.69
AXP 1RXS 1708-40 11.0
AXP 1E 1841-045 11.8
AXP AXJ1844-0258 6.97
AXP CXJ0110-7211 5.44
Please note that the second, fourth, and last names were abbreviated

SGR/AXP Online Catalog (An online catalog of SGR/AXP properties maintained by the pulsar group at McGill University)


Van Paradijs, J.; Taam, R. E.; Van Den Heuvel, E. P. J. (1995). "On the nature of the 'anomalous' 6-s X-ray pulsars". Astronomy and Astrophysics. 299: L41. Bibcode:1995A&A...299L..41V.
Duncan, Robert C.; Thompson, Christopher (1996). "Magnetars". AIP Conference Proceedings. 366. p. 111. doi:10.1063/1.50235.
Kouveliotou, Chryssa; Duncan, Robert C.; Thompson, Christopher (2003). "Magnetars" . Scientific American. 288 (2): 34. Bibcode:2003SciAm.288b..34K. doi:10.1038/scientificamerican0203-34. PMID 12561456.

External links

Meissner Effect in Quark Stars (University of Calgary)


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