A New Transient Source Observed by UHURU

Matilsky, T.; Giacconi, R.; Gursky, H.; Kellogg, E.; Tananbaum, H.

doi:10.1086/180947

Cited by 53 publications

(27 citation statements)

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“…The recurrent X-ray nova 4U 1543À47 was observed in outburst in 1971(Matilsky et al 1972Kitamoto et al 1984;Harmon et al 1992;this work). During the recent outburst, the peak X-ray intensity was 4.2 times that of the Crab Nebula (2-12 keV).…”

Section: Introductionmentioning

confidence: 50%

“…Nevertheless, we make a few comparisons, after setting aside the 1992 outburst, which was quite short-lived and observed only above 20 keV (Harmon et al 1992). For the three remaining outbursts, the spectra were very soft when the source was bright, and the peak X-ray intensities were 1.9 crab (2-6 keV) in 1971, 4.0 crab (3.7-7.5 keV) in 1983, and 3.3 crab (3.7-7.5 keV) on 2002 June 20 (Matilsky et al 1972;Kitamoto et al 1984;this work). During the bright outburst in 1983, the luminosity above 1.5 keV was 2:5 AE ð 0:3Þ ; 10 39 ergs s À1 for D ¼ 7:5 kpc (Kitamoto et al 1984), which nominally exceeds the Eddington luminosity of a 9.4 M black hole by a factor of 2.1.…”

Section: Comparison With Earlier Outbursts Of 4u 1543à47mentioning

confidence: 91%

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Spectral and Timing Evolution of the Black Hole X‐Ray Nova 4U 1543−47 during Its 2002 Outburst

Park

Miller

McClintock

et al. 2004

ApJ

155

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We present an X-ray spectral and timing analysis of 4U 1543À47 during its 2002 outburst based on 49 pointed observations obtained using the Rossi X-Ray Timing Explorer. The outburst reached a peak intensity of 4.2 crab in the 2-12 keV band and declined by a factor of 32 throughout the month-long observation. A 21:9 AE 0:6 mJy radio flare was detected at 1026.75 MHz two days before the X-ray maximum; the radio source was also detected late in the outburst, after the X-ray source entered the ''hard'' state. The X-ray light curve exhibits the classic shape of a rapid rise and an exponential decay. The spectrum is soft and dominated by emission from the accretion disk. The continuum is fitted with a multicolor disk blackbody (kT max ¼ 1:04 keV) and a power law (À $ 2:7). Midway through the decay phase, a strong low-frequency quasi-periodic oscillation ( ¼ 7:3 8:1 Hz) was present for several days. The spectra feature a broad Fe K line that is asymmetric, suggesting that the line is due to relativistic broadening rather than Comptonization. Relativistic Laor models provide much better fits to the line than nonrelativistic Gaussian models, particularly near the beginning and end of our observations. The line fits yield estimates for the inner disk radius that are within 6R g ; this result and additional evidence indicates that this black hole may have a nonzero angular momentum.

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Section: Introductionmentioning

confidence: 50%

Section: Comparison With Earlier Outbursts Of 4u 1543à47mentioning

confidence: 91%

Spectral and Timing Evolution of the Black Hole X‐Ray Nova 4U 1543−47 during Its 2002 Outburst

Park

Miller

McClintock

et al. 2004

ApJ

155

View full text Add to dashboard Cite

show abstract

“…This object was discovered by the Uhuru satellite on1971 August17 (Matilsky et al 1972). The source was observed again in outburst in 1983, in 1992, and also in 2002 (Kitamoto et al 1984;Harmon et al 1992;Miller & Remillard 2002;Brocksopp et al 2004).…”

Section: Introductionmentioning

confidence: 89%

Multiwavelength Observations of the Galactic Black Hole Transient 4U 1543−47 during Outburst Decay: State Transitions and Jet Contribution

Kalemci

Tomsick

Buxton

et al. 2005

ApJ

108

157

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Multiwavelength observations of Galactic black hole (GBH) transients during state transitions and in the low/hard state may provide detailed information on the accretion structure of these systems. The object 4U 1543À47 is a GBH transient that was covered exceptionally well in X-rays and the infrared (daily observations) and reasonably well in the optical and radio during its outburst decay in 2002. When all the available information is gathered from the intermediate and the low/hard states, 4U 1543À47 makes an important contribution to our understanding of state transitions and the role of outflows in the high-energy emission properties of black hole binaries. The evolution of the X-ray spectral and temporal properties and the infrared light curve place strong constraints on different models to explain the overall emission from accreting black holes. The overall spectral energy distribution is consistent with a synchrotron origin for the optical and infrared emission; however, the X-ray flux is above the power-law continuation of the optical and infrared flux. The infrared light curve, the HEXTE light curve, and the evolution of the X-ray photon index indicate that the major source of hard X-rays cannot be direct synchrotron radiation from an acceleration region in a jet for most of the outburst decay.

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“…In 4U 1543À47 these outbursts are recurrent with a quasi-period of 10-12 yr. Previous outbursts have been observed in 1971 (Matilsky et al 1972), 1983(Kitamoto et al 1984van der Woerd et al 1989(Harmon et al 1992, and 2002 (Park et al 2004;Kalemci et al 2005).…”

Section: Introductionmentioning

confidence: 96%

Fourier‐resolved Spectroscopy of 4U 1543−47 during the 2002 Outburst

Reig

Papadakis

Shrader

et al. 2006

ApJ

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We have obtained Fourier-resolved spectra of the black hole binary 4U 1543-47 in the canonical states (high/soft, very high, intermediate, and low/hard) observed in this source during the decay of an outburst that took place in 2002. Our objective is to investigate the variability of the spectral components generally used to describe the energy spectra of black hole systems, namely a disk component, a power-law component attributed to Comptonization by a hot corona, and the contribution of the iron line due to reprocessing of the high-energy (E k 7 keV ) radiation. We find that (1) the disk component is not variable on timescales shorter than $100 s, (2) the reprocessing emission as manifest by the variability of the Fe K line responds to the primary radiation variations down to timescales of $70 ms in the high and very high states, but longer than 2 s in the low state, (3) the low-frequency QPOs are associated with variations of the X-ray power-law spectral component and not to the disk component, and (4) the spectra corresponding to the highest Fourier frequency are the hardest (show the flatter spectra) at a given spectral state. These results question models that explain the observed power spectra as due to modulations of the accretion rate alone, as such models do not provide any apparent reason for a Fourier frequency dependence of the power-law spectral indices.

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A New Transient Source Observed by UHURU

Cited by 53 publications

References 0 publications

Spectral and Timing Evolution of the Black Hole X‐Ray Nova 4U 1543−47 during Its 2002 Outburst

Spectral and Timing Evolution of the Black Hole X‐Ray Nova 4U 1543−47 during Its 2002 Outburst

Multiwavelength Observations of the Galactic Black Hole Transient 4U 1543−47 during Outburst Decay: State Transitions and Jet Contribution

Fourier‐resolved Spectroscopy of 4U 1543−47 during the 2002 Outburst

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