High‐ and Low‐Frequency Quasi‐periodic Oscillations in the X‐Ray Light Curves of the Black Hole Transient H1743−322

Homan, J.; Miller, J. M.; Wijnands, Rudy; Klis, M. van der; Belloni, T.; Steeghs, D.; Lewin, W. H. G.

doi:10.1086/424994

Cited by 150 publications

(151 citation statements)

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“…The low-frequency as well as high frequency quasi-periodic oscillations (QPOs) along with a strong spectral variability are observed in the 2003 and other outbursts of the source in RXTE PCA data (Capitanio et al, 2005;Homan et al, 2005b;Kalemci et al, 2006;Prat et al, 2009;McClintock et al, 2009;Stiele et al, 2013). These have resemblance with several other typical Galactic black hole candidates (e.g., GRO J1655-40, XTE J1550-564, GX 339-4 etc.).…”

Section: Introductionmentioning

confidence: 88%

“…One can find After almost two decades, in 2003, the INTEGRAL satellite discovered signatures of renewed activity in hard X-rays (Revnivtsev et al, 2003) and later, RXTE also verified the presence of such an activity (Markwardt & Swank, 2003). During the 2003 outburst, the source was continuously and extensively monitored in X-rays (Parmar et al, 2003;Homan et al, 2005b;McClintock et al, 2009), IR (Steeghs et al, 2003), and in Radio bands (Rupen et al, 2003) to reveal the multi-wavelength properties of the source. The multiwavelength campaign on this source during its 2003 and 2009 outbursts were also carried out by McClintock et al (2009);Miller-Jones et al (2012) respectively.…”

Section: Introductionmentioning

confidence: 99%

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Evolution of the temporal and the spectral properties in 2010 and 2011 outbursts of H 1743-322

Debnath

Chakrabarti

Nandi

2013

Advances in Space Research

111

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The Galactic black hole candidate H 1743-322 exhibited two X-ray outbursts in rapid succession: one in August 2010 and the other in April 2011. We analyze archival data of this object from the PCA instrument on board RXTE (2-25 keV energy band) to study the evolution of its temporal and spectral characteristics during both the outbursts, and hence to understand the behavioral change of the accretion flow dynamics associated with the evolution of the various X-ray features. We study the evolution of QPO frequencies during the rising and the declining phases of both the outbursts. We successfully fit the variation of QPO frequency using the Propagating Oscillatory Shock (POS) model in each of the outbursts and obtain the accretion flow parameters such as the instantaneous shock locations, the shock velocity and the shock strength. Based on the degree of importance of the thermal (disk black body) and the non-thermal (power-law) components of the spectral fit and properties of the QPO (if present), the entire profiles of the 2010 and 2011 outbursts are subdivided into four different spectral states: hard, hard-intermediate, soft-intermediate and soft. We attempt to explain the nature of the outburst profile (i.e., hardness-intensity diagram) with two different types of mass accretion flow.

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Section: Introductionmentioning

confidence: 88%

Section: Introductionmentioning

confidence: 99%

Evolution of the temporal and the spectral properties in 2010 and 2011 outbursts of H 1743-322

Debnath

Chakrabarti

Nandi

2013

Advances in Space Research

111

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“…Four sources (GRO J1655-40, XTE J1550-564, GRS 1915+105, and H1743-322) exhibit pairs of QPOs that have commensurate frequencies in a 3:2 ratio (Remillard et al 2002;Homan et al 2005;Remillard et al 2005;McClintock et al 2005). All of these HFQPOs have frequencies above 100 Hz.…”

Section: High-frequency Qpos From Black Hole Binariesmentioning

confidence: 99%

“…In the case of H1743-322, there are very few HFQPO detections in individual observations (Homan et al 2005;Remillard et al 2005). However, the technique used to combine observations to gain some of the HFQPO detections at 2ν 0 and 3ν 0 utilized SPL classifications grouped by luminosity level.…”

Section: High-frequency Qpos and The Spl Statementioning

confidence: 99%

X‐ray spectral states and high‐frequency QPOs in black holebinaries

Remillard

2005

Astron Nachr

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Abstract. The high-frequency quasi-periodic oscillations (HFQPOs) in the X-ray emission of black hole binaries and candidates are briefly reviewed with respect to the question of X-ray states. We use the prescription of McClintock and Remillard (2005), in which X-ray spectra and power density spectra are used to differentiate three main states of active accretion: "thermal", "hard", and "steep power-law". Respectively, each state emphasizes a different physical element that may contribute radiation: the accretion disk, a jet, and a compact non-thermal corona. We focus on the four sources that exhibit pairs of HFQPOs with frequencies that scale in a 3:2 ratio. All of these HFQPOs are associated with the steep power-law (SPL) state. Furthermore, there is a clear trend in which the 2ν0 oscillation is seen when the source has high X-ray luminosity, while the 3ν0 QPO is seen at lower luminosity.

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“…The most interesting HFQPOs is the 3:2 HFQPO pairs observed in a few BH binaries, e.g., GRO J1655−40 (450, 300 Hz; Remillard et al 1999;Strohmayer 2001;Remillard et al 2002Miller et al 2001;Remillard et al 2002) andGRS 1915 + 105 (168, 113 Hz;RM06). Furthermore, the 3:2 HFQPO pair has been observed in the bright X-ray transient H1743−322 (240, 160 Hz;Homan et al 2005;, although the mass of its BH primary has not been measured (RM06). vere damping forces and emit X-rays with sufficient amplitude and coherence to produce the HFQPOs (e.g.…”

Section: Introductionmentioning

confidence: 99%

A model for 3:2 HFQPO pairs in black hole binaries based on cosmic battery

Huang¹,

Ye²,

Wang³

et al. 2016

Mon. Not. R. Astron. Soc.

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A model for 3:2 high-frequency quasi-periodic oscillations (HFQPOs) with 3:2 pairs observed in four black hole X-ray binaries (BHXBs) is proposed by invoking the epicyclic resonances with the magnetic connection (MC) between a spinning black hole (BH) with a relativistic accretion disc. It turns out that the MC can be worked out due to Poynting-Robertson cosmic battery (PRCB), and the 3:2 HFQPO pairs associated with the steep power-law states can be fitted in this model. Furthermore, the severe damping problem in the epicyclic resonance model can be overcome by transferring energy from the BH to the inner disc via the MC process for emitting X-rays with sufficient amplitude and coherence to produce the HFQPOs. In addition, we discuss the important role of the magnetic field in state transition of BHXBs.

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High‐ and Low‐Frequency Quasi‐periodic Oscillations in the X‐Ray Light Curves of the Black Hole Transient H1743−322

Cited by 150 publications

References 40 publications

Evolution of the temporal and the spectral properties in 2010 and 2011 outbursts of H 1743-322

Evolution of the temporal and the spectral properties in 2010 and 2011 outbursts of H 1743-322

X‐ray spectral states and high‐frequency QPOs in black holebinaries

A model for 3:2 HFQPO pairs in black hole binaries based on cosmic battery

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