SAX J1808.4−3658: Difference between revisions
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A transient X-ray source first discovered in 1996 by the Italian [[BeppoSAX]] satellite, '''SAX J1808.4-3658''' revealed X-ray pulsations at the 401 Hz neutron star spin frequency when it was observed during a subsequent outburst in 1998 by [[NASA]]'s [[Rossi X-ray Timing Explorer|RXTE]] satellite. The [[neutron star]] orbits a [[brown dwarf]] binary companion every 2.01 hours. |
A transient X-ray source first discovered in 1996 by the Italian [[BeppoSAX]] satellite, '''SAX J1808.4-3658''' revealed X-ray pulsations at the 401 Hz neutron star spin frequency when it was observed during a subsequent outburst in 1998 by [[NASA]]'s [[Rossi X-ray Timing Explorer|RXTE]] satellite. The [[neutron star]] orbits a [[brown dwarf]] binary companion every 2.01 hours. [[X-ray burster|X-ray burst]] oscillations and quasi-periodic oscillations in addition to coherent X-ray pulsations have been seen from SAX J1808.4-3658, making it a Rosetta stone for interpretation of the timing behavior of [[low-mass X-ray binary|low-mass X-ray binaries]]. |
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These [[pulsar]]s are thought to be the evolutionary progenitors of recycled [[millisecond pulsar|millisecond pulsars]]. A total of seven accreting millisecond X-ray pulsars have been discovered as of October 2006. |
These accreting millisecond X-ray [[pulsar]]s are thought to be the evolutionary progenitors of recycled radio [[millisecond pulsar|millisecond pulsars]]. A total of seven accreting millisecond X-ray pulsars have been discovered as of October 2006. |
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Revision as of 03:49, 25 October 2006
Template:Astrobox begin2 Template:Star listings Template:Astrobox end A transient X-ray source first discovered in 1996 by the Italian BeppoSAX satellite, SAX J1808.4-3658 revealed X-ray pulsations at the 401 Hz neutron star spin frequency when it was observed during a subsequent outburst in 1998 by NASA's RXTE satellite. The neutron star orbits a brown dwarf binary companion every 2.01 hours. X-ray burst oscillations and quasi-periodic oscillations in addition to coherent X-ray pulsations have been seen from SAX J1808.4-3658, making it a Rosetta stone for interpretation of the timing behavior of low-mass X-ray binaries.
These accreting millisecond X-ray pulsars are thought to be the evolutionary progenitors of recycled radio millisecond pulsars. A total of seven accreting millisecond X-ray pulsars have been discovered as of October 2006.
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