Anomalous X-Ray Pulsar: Difference between revisions
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[[File:Anomalous X- | [[File:Anomalous X-ray Pulsar.jpg|thumb|250px|right|An Anomalous X-ray Pulsar.jpg]] | ||
[[Anomalous X-Ray Pulsar]]s (AXPs) are now widely believed to be [[Magnetar]]s —young, isolated, highly magnetized [[Neutron Star]]s. These energtic X-ray pulsars are characterized by slow rotation periods of ~2–12 seconds and large magnetic fields of ~1013–1015 [[Gauss]] (1 to 100 [[Tesla|Gigatesla]]s). There are currently 9 known and 1 candidate AXPs. The identification of AXPs with magnetars was motivated by their similarity to another enigmatic class of sources, the [[Soft Gamma Repeater]]s. | [[Anomalous X-Ray Pulsar]]s (AXPs) are now widely believed to be [[Magnetar]]s —young, isolated, highly magnetized [[Neutron Star]]s. These energtic X-ray pulsars are characterized by slow rotation periods of ~2–12 seconds and large magnetic fields of ~1013–1015 [[Gauss]] (1 to 100 [[Tesla|Gigatesla]]s). There are currently 9 known and 1 candidate AXPs. The identification of AXPs with magnetars was motivated by their similarity to another enigmatic class of sources, the [[Soft Gamma Repeater]]s. | ||
Latest revision as of 15:54, 9 March 2010
Anomalous X-Ray Pulsars (AXPs) are now widely believed to be Magnetars —young, isolated, highly magnetized Neutron Stars. These energtic 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 9 known and 1 candidate AXPs. The identification of AXPs with magnetars was motivated by their similarity to another enigmatic class of sources, the Soft Gamma Repeaters.
