In this paper, we report on radio (Very Large Array and Austrialian Telescope Compact Array) and X-ray (RXTE, Chandra and Swift) observations of the outburst decay of the transient black hole candidate H 1743-322 in early 2008. We find that the X-ray light curve followed an exponential decay, levelling off towards its quiescent level. The exponential decay time-scale is approximate to 4 days and the quiescent flux corresponds to a luminosity of 3 x 10(32)(d/7.5kpc)(2)erg s(-1). This together with the relation between quiescent X-ray luminosity and orbital period reported in the literature suggests that H 1743-322 has an orbital period longer than approximate to 10 h. Both the radio and X-ray light curve show evidence for flares. The radio-X-ray correlation can be well described by a power-law with index approximate to 0.18. This is much lower than the index of approximate to 0.6-0.7 found for the decay of several black hole transients before. The radio spectral index measured during one of the radio flares while the source is in the low-hard state is -0.5 +/- 0.15, which indicates that the radio emission is optically thin. This is unlike what has been found before in black hole sources in the low-hard state. We attribute the radio flares and the low index for the radio-X-ray correlation to the presence of shocks downstream the jet flow, triggered by ejection events earlier in the outburst. We find no evidence for a change in X-ray power-law spectral index during the decay, although the relatively high extinction of N-H appro...
Low-hard State Quiescent X-ray Luminosity Black Hole Transients Black Hole Sources Black Hole Candidate Black Hole Decay Of Transients X-ray Light Curve Quiescent Level Radio Flares
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Climate change Research Articles published between Jan 23, 2023 to Jan 29, 2023
Jan 30, 2023
Articles Included: 3
Climate change adaptation has shifted from a single-dimension to an integrative approach that aligns with vulnerability and resilience concepts. Adapt...Read More
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