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J. H. Swank (NASA/GSFC), C. B. Markwardt (UMD, NASA/GSFC), M. P. Rupen (NAS/NRC, NASA/GSFC, NRAO), A. J. Mioduszewski, V. Dhawan (NRAO)
The black hole candidate X-ray transient H1743-322 = IGR J1746-3213 = XTE J17464-3213 had a bright outburst starting in March 2003, which reached a peak flux around 1.3 Crab and lasted nearly 2/3 of a year. After a similar period in apparent quiescence (below ~1 mCrab), the source began another outburst in July 2004, this time rising only to about 1/4 Crab and decaying in about 4.5 months. It appeared with an optically thick disk and a steep power law component (number index ~ 3), and began a steady increase, with mild spectral change. After 50 days, a hard power-law component appeared, along with low frequency quasiperiodic oscillations. Gradual decay of both components began, but after another month the soft component dropped faster and left the harder component to dominate the decay. However, transition to a low hard state like that of Cygnus X-1 had still not occurred. The Very Large Array found no radio activity during the first month, but a 2 mJy radio source appeared during the X-ray rise. Evidence for jet ejection corresponding to changes in the X-ray source will be discussed in connection with interpretation of the system.
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Bulletin of the American Astronomical Society, 36 5
© 2004. The American Astronomical Society.