The complex behaviour of the microquasar GRS 1915+105 in the<i>ρ</i>class observed with BeppoSAX

Massaro, E.; Ventura, G.; Massa, F.; Feroci, M.; Mineo, T.; Cusumano, G.; Casella, P.; Belloni, T.

doi:10.1051/0004-6361/200912908

Cited by 22 publications

(37 citation statements)

References 38 publications

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“…Other authors (Janiuk & Czerny 2005;Massaro et al 2010) have already demonstrated that there is typically a delay between the soft and hard X-ray pulses as well as a strong relationship between the times between these two bursts and the cycle period. Because HR1 peaks at the hard pulse, we see that the hard Xray pulse lags the soft X-ray pulse by an average of 3.3 s in our observation.…”

Section: Phase Ephemeris and Folded Light Curvementioning

confidence: 92%

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The Physics of the “Heartbeat” State of GRS 1915+105

Neilsen

Remillard

Lee

2011

ApJ

158

282

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We present the first detailed phase-resolved spectral analysis of a joint Chandra High-Energy Transmission Grating Spectrometer and Rossi X-ray Timing Explorer observation of the ρ variability class in the microquasar GRS 1915+105. The ρ cycle displays a high-amplitude, double-peaked flare that recurs roughly every 50 s and is sometimes referred to as the "heartbeat" oscillation. The spectral and timing properties of the oscillation are consistent with the radiation pressure instability and the evolution of a local Eddington limit in the inner disk. We exploit strong variations in the X-ray continuum, iron emission lines, and the accretion disk wind to probe the accretion geometry over nearly six orders of magnitude in distance from the black hole. At small scales (1-10 R g ), we detect a burst of bremsstrahlung emission that appears to occur when a portion of the inner accretion disk evaporates due to radiation pressure. Jet activity, as inferred from the appearance of a short X-ray hard state, seems to be limited to times near minimum luminosity, with a duty cycle of ∼10%. On larger scales (10 5 -10 6 R g ), we use detailed photoionization arguments to track the relationship between the fast X-ray variability and the accretion disk wind. For the first time, we are able to show that changes in the broadband X-ray spectrum produce changes in the structure and density of the accretion disk wind on timescales as short as 5 s. These results clearly establish a causal link between the X-ray oscillations and the disk wind and therefore support the existence of a disk-jet-wind connection. Furthermore, our analysis shows that the mass-loss rate in the wind may be sufficient to cause long-term oscillations in the accretion rate, leading to state transitions in GRS 1915+105.

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Section: Phase Ephemeris and Folded Light Curvementioning

confidence: 92%

“…HR1 looks rather like the mirror image of the count rate (i.e., flipped horizontally about its maximum), except that HR1 is typically single-peaked. Other instances of the ρ state have shown different behaviors, as the number and relative strengths of the peaks can vary (Massaro et al 2010;J. Neilsen et al 2011, in preparation).…”

Section: Timing Analysismentioning

confidence: 99%

The Physics of the “Heartbeat” State of GRS 1915+105

Neilsen

Remillard

Lee

2011

ApJ

158

282

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“…It has been shown that hard X-ray photons tend to lag soft ones in this class (e.g. Janiuk & Czerny 2005;Massaro et al 2010). Numerical models derived from Shakura & Sunyaev 1973 which reproduce this lag can also reproduce other flaring classes seen in GRS 1915 (e.g Nayakshin et al 2000;Massaro et al 2014).…”

Section: Introductionmentioning

confidence: 99%

An atlas of exotic variability in IGR J17091−3624: a comparison with GRS 1915+105

Court

Altamirano

Pereyra

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We performed an analysis of all RXTE observations of the Low Mass X-ray Binary and Black Hole Candidate IGR J17091-3624 during the 2011-2013 outburst of the source. By creating lightcurves, hardness-intensity diagrams and power density spectra of each observation, we have created a set of 9 variability 'classes' that phenomenologically describe the range of types of variability seen in this object. We compare our set of variability classes to those established by Belloni et al. (2000) to describe the similar behaviour of the LMXB GRS 1915+105, finding that some types of variability seen in IGR J17091-3624 are not represented in data of GRS 1915+105. We also use all available X-ray data of the 2011-2013 outburst of IGR J17091-3624 to analyse its longterm evolution, presenting the first detection of IGR J17091-3624 above 150 keV as well as noting the presence of 're-flares' during the latter stages of the outburst. Using our results we place new constraints on the mass and distance of the object, and find that it accretes at 33% of its Eddington limit. As such, we conclude that Eddingtonlimited accretion can no longer be considered a sufficient or necessary criterion for GRS 1915+105-like variability to occur in Low Mass X-Ray Binaries.

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“…The ρ class (heartbeat state) is a peculiar class where the source oscillates quasi-periodically between states B and C. The light curves in the ρ class have one to several peaks per ρ-cycle (e.g. Taam et al 1997;Vilhu & Nevalainen 1998;Belloni et al 2000;Massaro et al 2010). We call the ρ class with one peak per cycle the single-peaked ρ class (hereafter called ρ1 class), and the ρ class with two peaks per cycle the double-peaked ρ class (hereafter called ρ2 class).…”

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confidence: 99%

A timing view of the heartbeat state of GRS 1915+105

Yan

Méndez

et al. 2016

Mon. Not. R. Astron. Soc.

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We present a timing analysis of two Rossi X-ray Timing Explorer observations of the microquasar GRS 1915+105 during the heartbeat state. The phase-frequency-power maps show that the intermediate-frequency aperiodic X-ray variability weakens as the source softens in the slow rise phase, and when the quasi-periodic oscillation disappears in the rise phase of the pulse of the double-peaked class its sub-harmonic is still present with a hard phase lag. In the slow rise phase, the energy-frequency-power maps show that most of the aperiodic variability is produced in the corona, and may also induce the aperiodic variability observed at low energies from an accretion disk, which is further supported by the soft phase lag especially in the intermediate-frequency range (with a time delay up to 20 ms). In the rise phase of the pulse, the low-frequency aperiodic variability is enhanced significantly and there is a prominent hard lag (with a time delay up to 50 ms), indicating that the variability is induced by extension of the disk toward small radii as implied by the increase in flux and propagates into the corona. However, during the hard pulse of the double-peaked class, the variability shows no significant lag, which may be attributed to an optically thick corona. These timing results are generally consistent with the spectral results presented by Neilsen et al. (2011Neilsen et al. ( , 2012 which indicated that the slow rise phase corresponds to a local Eddington limit and the rise phase of the pulse corresponds to a radiation pressure instability in the disk.

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The complex behaviour of the microquasar GRS 1915+105 in theρclass observed with BeppoSAX

Cited by 22 publications

References 38 publications

The Physics of the “Heartbeat” State of GRS 1915+105

The Physics of the “Heartbeat” State of GRS 1915+105

An atlas of exotic variability in IGR J17091−3624: a comparison with GRS 1915+105

A timing view of the heartbeat state of GRS 1915+105

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