Editing Anomalous X-Ray Pulsar
Warning: You are not logged in. Your IP address will be publicly visible if you make any edits. If you log in or create an account, your edits will be attributed to your username, along with other benefits.
The edit can be undone. Please check the comparison below to verify that this is what you want to do, and then publish the changes below to finish undoing the edit.
Latest revision | Your text | ||
Line 1: | Line 1: | ||
[[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. |