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[update]) 12 confirmed and 2 candidate AXPs. 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|
|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.
- Meissner Effect in Quark Stars (University of Calgary)
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