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A transient X-ray source first discovered in 1996 by the Italian-Dutch 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 is orbited by a brown dwarf binary companion with a likely mass of 0.05 solar masses, 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.

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  • SAX J1808.4−3658 (en)
  • SAX J1808.4-3658 (pt)
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  • A transient X-ray source first discovered in 1996 by the Italian-Dutch 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 is orbited by a brown dwarf binary companion with a likely mass of 0.05 solar masses, 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. (en)
  • Uma fonte de raios-X transitória foi descoberta em 1996 pelo satélite italiano-holandês BeppoSAX, SAX J1808.4-3658 revelou pulsações de raios-X em 401 Hz, freqüência de rotação de estrelas de nêutrons quando foi observada durante uma explosão subseqüente em 1998 pelo satélite NASA RXTE. Um total de dez milisegundos de raios-X pulsares foram descobertos em outubro de 2007. Três deles são intermitentes milisegundos pulsares de raios-X (HETE J1900.1-2455, Aql X-1 e SAX J1748.9-2021), ou seja, eles emitem pulsações esporadicamente durante a explosão. (pt)
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  • SAX J1808.4−3658 (en)
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  • http://commons.wikimedia.org/wiki/Special:FilePath/V4580SgrLightCurve.png
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  • V4580 Sgr, PSR J1808−3658, SWIFT J1808.5−3655, INTREF 881, XTE J1808−369 (en)
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  • SAX+J1808.4-3658 (en)
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  • A transient X-ray source first discovered in 1996 by the Italian-Dutch 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 is orbited by a brown dwarf binary companion with a likely mass of 0.05 solar masses, 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 thirteen accreting millisecond X-ray pulsars have been discovered as of January 2011. Three of them are Intermittent millisecond X-ray pulsars (HETE J1900.1-2455, Aql X-1 and SAX J1748.9-2021), i.e. they emit pulsations sporadically during the outburst. On 21 August 2019 (UTC; 20 August in the US), Neutron Star Interior Composition Explorer (NICER) spotted the brightest X-ray burst so far observed. It came from SAX J1808.4−3658. (en)
  • Uma fonte de raios-X transitória foi descoberta em 1996 pelo satélite italiano-holandês BeppoSAX, SAX J1808.4-3658 revelou pulsações de raios-X em 401 Hz, freqüência de rotação de estrelas de nêutrons quando foi observada durante uma explosão subseqüente em 1998 pelo satélite NASA RXTE. Quando foi observado durante uma posterior explosão em 1998 pela NASA's RXTE satélite. A estrela de nêutrons orbita uma anã castanha binário com um companheiro provável massa de 0,05 massas solares, a cada 2,01 horas. Raio-X tendo oscilações quase-periódico, além de coerente de raios-X pulsações ter sido visto a partir de SAX J1808.4-3658, tornando-se uma Pedra de Roseta para a interpretação do calendário de comportamento de baixa massa de raios-X binários. Um total de dez milisegundos de raios-X pulsares foram descobertos em outubro de 2007. Três deles são intermitentes milisegundos pulsares de raios-X (HETE J1900.1-2455, Aql X-1 e SAX J1748.9-2021), ou seja, eles emitem pulsações esporadicamente durante a explosão. (pt)
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