High-frequency quasi-periodic oscillations from GRS 1915+105 in its C state

Belloni, T.; Soleri, P.; Casella, P.; Méndez, Mariano; Migliari, S.

doi:10.1111/j.1365-2966.2006.10286.x

Cited by 55 publications

(57 citation statements)

References 25 publications

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“…Figure 13 shows the power-law tail of the observed flux for the HS and coronal emission. The simulation gives a photon index close to the one observed For GRS 1915+105 by Belloni et al (2006) in the SPL state. The phase-resolved energy spectra of the HS and the accretion disk are shown in Figure 14.…”

Section: Thermal Emissionsupporting

confidence: 75%

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Studies of the Origin of High-Frequency Quasi-Periodic Oscillations of Mass-Accreting Black Holes in X-Ray Binaries With Next-Generation X-Ray Telescopes

Beheshtipour

Hoormann

Krawczynski

2016

ApJ

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Observations with RXTE (Rossi X-ray Timing Explorer) revealed the presence of high-frequency quasi-periodic oscillations (HFQPOs) of the X-ray flux from several accreting stellar-mass black holes. HFQPOs (and their counterparts at lower frequencies) may allow us to study general relativity in the regime of strong gravity. However, the observational evidence today does not yet allow us to distinguish between different HFQPO models. In this paper we use a general-relativistic ray-tracing code to investigate X-ray timing spectroscopy and polarization properties of HFQPOs in the orbiting Hotspot model. We study observational signatures for the particular case of the 166 Hz quasi-periodic oscillation (QPO) in the galactic binary GRS1915+105. We conclude with a discussion of the observability of spectral signatures with a timing-spectroscopy experiment such as the LOFT (Large Observatory for X-ray Timing) and polarization signatures with space-borne X-ray polarimeters such as IXPE (Imaging X-ray Polarimetry Explorer), PolSTAR (Polarization Spectroscopic Telescope Array), PRAXyS (Polarimetry of Relativistic X-ray Sources), or XIPE (X-ray Imaging Polarimetry Explorer). A mission with high count rate such as LOFT would make it possible to get a QPO phase for each photon, enabling the study of the QPO-phase-resolved spectral shape and the correlation between this and the flux level. Owing to the short periods of the HFQPOs, first-generation X-ray polarimeters would not be able to assign a QPO phase to each photon. The study of QPO-phase-resolved polarization energy spectra would thus require simultaneous observations with a first-generation X-ray polarimeter and a LOFT-type mission.

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Section: Thermal Emissionsupporting

confidence: 75%

“…The vertical optical depth of this layer is set to a constant, τ 0 =0.2, and the temperature of the hot electrons in the corona is set to T corona =30 keV. These parameters reproduce the observed photon index for GRS 1915+105 in the SPL state (Belloni et al 2006). The opening angle of the wedge is set to 2°.…”

Section: Corona Simulationmentioning

confidence: 99%

Studies of the Origin of High-Frequency Quasi-Periodic Oscillations of Mass-Accreting Black Holes in X-Ray Binaries With Next-Generation X-Ray Telescopes

Beheshtipour

Hoormann

Krawczynski

2016

ApJ

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“…That the fourth state (the one with both LF and HF QPO) was observed in this source by Belloni et al (2006) is important as it gives support to and confidence in our tentative classification.…”

Section: Observations Of a State With Both Hf And Lf Qpossupporting

confidence: 63%

“…The main difference from the classification of Belloni et al (2000), based on GRS 1915+105, is that we separate their C state into two (AEI-dominated state and AEI-RWIdominated state), depending on the high frequency variability. Since this classification was first proposed, we have learned that HFQPOs occur in the C state as defined by Belloni et al (2000) (see Belloni et al 2006), so the AEI-MRI-dominated state has been observed in GRS 1915+105.…”

Section: A Model Independent Look At the Classificationmentioning

confidence: 99%

A microquasar classification from a disk instability perspective

Tagger

Rodríguez

2010

A&A

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Aims. The spectacular variability of microquasars has led to many efforts to classify their observed behaviors in a few states. The progress made in the understanding of the quasi-periodic oscillations observed in these objects now makes it possible to develop a new way of identifying order in their behavior, based on the theorized physical processes associated with these oscillations. This development will also help us to reunite microquasars in a single classification based on the physical processes at work and therefore independent of their specific properties (mass, variation timescale, outburst history, etc.). This classification is intended to be a tool to improve our understanding of microquasar behavior and not to replace phenomenological states. Methods. We start by considering three instabilities that can cause accretion in the disk. We compare the conditions for their development, and the quasi-periodic oscillations they can be expected to produce, with the spectral states in which these quasi-periodic oscillations are observed and sometimes coexist. Results. From the three instabilities that we proposed to explain the three states of GRS 1915+105 we actually found the theoretical existence of four states. We compared those four states with observations and also how those four states can be seen in a model-independent fashion. Those four state can be used to find an order in microquasar observations, based on the properties of the quasi-periodic oscillations and the physics of the associated instabilities.

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“…A high-frequency QPO was discovered in GRS 1915+105 during the θ class of variability by Belloni et al (2006); more recently Mikles et al (2009) showed that during the same class the color radius-frequency relation was different from the standard Keplerian one, and that the points were on the left side of the theoretical plot of Fig. 1.…”

Section: Grs 1915+105mentioning

confidence: 97%

A possible interpretation for the apparent differences in LFQPO types in microquasars

Varnière

Tagger

Rodríguez

2012

A&A

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Aims. In most microquasars, low-frequency quasi-periodic oscillations (LFQPO) have been classified into three types (A, B and C depending on the peak distribution in the power density spectra and the shape of the noise) but no explanation has been proposed yet. The accretion-ejection instability (AEI) was presented in 1999 as a possible explanation for the fast varying LFQPO that occur most often. Here we look at a possible generalization to explain the characteristics of the other two LFQPO types. Methods. It was recently shown that when the disk approaches its last stable orbit, the AEI is markedly affected by relativistic effects. We focus on the characteristics of the LFQPO that would result from the relativistic AEI and compare them with the different LFQPO types. Results. The effects of relativity on the AEI seem to be able to explain most of the characteristics of the three types of LFQPO within one formalism.

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High-frequency quasi-periodic oscillations from GRS 1915+105 in its C state

Cited by 55 publications

References 25 publications

Studies of the Origin of High-Frequency Quasi-Periodic Oscillations of Mass-Accreting Black Holes in X-Ray Binaries With Next-Generation X-Ray Telescopes

Studies of the Origin of High-Frequency Quasi-Periodic Oscillations of Mass-Accreting Black Holes in X-Ray Binaries With Next-Generation X-Ray Telescopes

A microquasar classification from a disk instability perspective

A possible interpretation for the apparent differences in LFQPO types in microquasars

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