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The spectral and temporal evolution during X-ray outbursts give importantclues on the accretion process and radiation mechanism in black-hole X-raybinaries (BH XRBs). A set of Swift and RXTE observations were executed tomonitor the 2008 outburst of the black-hole candidate Swift J1842.5-1124. Weinvestigate these data to explore the accretion physics in BH XRBs. We carryout a comprehensive spectral and timing analysis on all the available pointingobservations, including fitting both X-ray spectra and power density spectra,measuring the optical and near-ultraviolet flux density. We also search forcorrelations among the spectral and timing parameters. The observed propertiesof Swift J1842.5-1124 are similar to other BH XRBs in many respects, forexample the hardness-intensity diagram and hardness-rms diagram. The type-Cquasi-periodic oscillations (QPOs) were observed as the source started totransit from the low-hard state to the high-soft state. The frequency of QPOscorrelate with intensity and the hard component index, and anti-correlate withthe hardness and the total fractional rms. These relations are consistent withthe Lense-Thirring precession model. The estimated U-band flux changed with theX-ray flux, while the flux density at the V band remained 0.26 mJy. Theseresults imply that the X-ray reprocessing or the tail of thermal emission fromthe outer disk contributes a significant fraction of the U-band radiation;alternatively, the companion star or the jet dominates the flux at longerwavelengths.

The X-ray view of black-hole candidate Swift J1842.5-1124 during its 2008 outburst