The evolution of the timing properties of the black-hole transient GX 339-4 during its 2002/2003 outburst

By T. Belloni, J. Homan, P. Casella, M. van der Klis, E. Nespoli, W. Lewin, J. Miller, M. INAF-OAB, Italy., Mit and 5 more. 2005

366 citations recorded by the source corpus.

We present the results of the timing and color analysis of more than two hundred RXTE/PCA observations of the bright black-hole transient GX 339-4 obtained during its 2002/2003 outburst. The color-intensity evolution of the system, coupled to the properties of its fast time variability, allow the identification of four separate states. Depending on the state, strong noise is detected, together with a variety of quasi-periodic oscillations at frequencies from 0.2 to 8 Hz. We present a characterization of the timing parameters of these states and compare them to what has been observed in other systems. These results, together with those obtained from energy spectra, point towards a common evolution of black-hole transients through their outbursts.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/f262265ffed36bb2c8593ee4f4d5c0bd7d47734d

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Nuclear and High Energy Physics

Citations in the corpus

WATCHDOG: A COMPREHENSIVE ALL-SKY DATABASE OF GALACTIC BLACK HOLE X-RAY BINARIES (2015, background): “The basic “turtlehead” pattern presented above has been modelled after numerous outbursts of GX 339−4 (Zdziarski et al. 2004; Fender et al. 2004; Belloni et al. 2005; Homan & Belloni 2005; Del Santo et al. 2008; Belloni 2010; Motta et al. 2009; Corbel et al. 2013; Debnath et al. 2013b) and can be…”
Going with the Flow: Can the Base of Jets Subsume the Role of Compact Accretion Disk Coronae? (2005, background): “(They do not, however, encompass the most extreme bright and relatively soft HS data discussed by Homan et al. 2005, Nowak et al. 2005, and Belloni et al. 2005.)”
A review of quasi-periodic oscillations from black hole X-ray binaries: Observation and theory (2019, background): “Typical bounds for the hard and soft bands are ∼ 6−10 keV and 4−6 keV [23], but being rather arbitrarily chosen, the ranges used vary quite a lot across different studies and different instruments.”
Low-frequency oscillations in black holes: a spectral-timing approach to the case of GX 339-4 (2011, background): “…carried out by RXTE during the 2002, 2004, 2007 and 2010 outburst has yielded detailed studie on the evolution of black hole states throughout the outburst (see e.g. Belloni et al. 2005), making the source an ideal candidate for an extensive study on the spectral-timing properties of BHBs.”
Ultraluminous X-ray sources in the Chandra and XMM-Newton era (2011, methodology): “Similar behavior has been seen from Galactic BHBs in the hard state (Belloni et al. 2005; Remillard & McClintock 2006).”
Jets from black hole X-ray binaries: testing, refining and extending empirical models for the coupling to X-rays (2009, background): “The study of GX 339-4 reported in Belloni et al. (2005) implies that the lower-luminosity outburst of GX 339-4 in 2004–5 made the ’hard intermediate state’ (HIMS) to ’soft intermediate state’ (SIMS) transition at a larger hardness ratio than theoutburst in 2002–03.”
Accretion states and radio loudness in active galactic nuclei: analogies with X-ray binaries (2006, methodology): “Additionally, the timing properties of the X-ray light curve change dramatically with the position in the HID (e.g. Homan et al. 2001; Belloni et al. 2005; Remillard 2005).”
The 'universal' radio/X-ray flux correlation : the case study of the black hole GX 339-4 (2012, neutral): “Since then, seven outbursts were observed: 2002- 03 (Homan et al. 2005; Belloni et al. 2005), 2004-05 (Belloni et al. 2006), 2006, 2007 (e.g. Tomsick et al. 2008), 2008, 2009, 2010-11 (Shidatsu et al. 2011; Cadolle Bel et al. 2011; Motta et al. 2011; Rahoui et al. 2012) and a temporary reactivation…”
Intrinsic disc emission and the soft X‐ray excess in active galactic nuclei (2011, background): “Spectra from this latter state appear very similar to intermediate spectra seen as the source makes a transition from the low/hard to high/soft states (e.g. Belloni et al 2005).”
A global spectral study of black hole X-ray binaries (2009, background): “…(2001) , (3)Tomsick & Kaaret (2000) , (4) Kalemci (2002) , (5) Brocksopp et al. (2006) , (6) Debnath et al. (2008) , (7) Nowak et al. (2002) , (8) Belloni et al. (2005) , (9) Belloni et al. (2006) , (10) Kalemci et al. (2006) , (11) Homan et al. (2001) , (12) Miller et al. (2001) , (13)…”
X-Ray Properties of Black-Hole Binaries (2006, background): “It is therefore a frequent target for radio studies (e.g., Fender et al. 1999; Corbel et al. 2000; Gallo et al. 2003; Belloni et al. 2005).”
Modelling the behaviour of accretion flows in X-ray binaries (2007, background): “However, there are also systematic correlations in the width and rms of these components, such that as each component approaches ∼ 5 Hz its amplitude and width drops (Pottschmidt et al. 2003; Kalemci et al. 2004; Belloni et al. 2005; Axelsson et al. 2005; Kalemci et al. 2006).”
A synthesis model for AGN evolution: supermassive black holes growth and feedback modes (2008, background): “…the many analogies between the high-energy spectra 1 In fact, the overall evolution of transient black holes doesshow clear evidences of hysteresis (Miyamoto et al. 1995; Belloni et al. 2005), with the intermediate spectral states having different luminositywhen sources enter or leave the outburst.”