Anomalous X-ray pulsar
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 2009) 9 known and 1 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 | ||
References
- ↑ SGR/AXP Online Catalog (An online catalog of SGR/AXP properties maintained by the pulsar group at McGill University)
External links
- Meissner Effect in Quark Stars (University of Calgary)
- "Magnetars" (Paper from a March 1995 conference proceedings, with first use of the term "AXP" and suggestion that AXPs are magnetars.)
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