Comparing theρandχclass spectra of the microquasar GRS 1915+105 observed withBeppoSAX

Mineo, T.; Massaro, E.; Massa, F.; D’Aí, A.

doi:10.1051/0004-6361/201629657

Cited by 4 publications

(5 citation statements)

References 48 publications

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“…The idea that the QPO originates from the corona is also consistent with the fact that the QPO absolute amplitude is low at the pulse phase (Fig. 1) where the corona flux is at its minimum (Mineo et al 2012(Mineo et al , 2017, and with the result that both the QPO absolute amplitude and the corona flux at phase below ∼ 0.85 are coincidentally higher in the ρ2 class than in the ρ1 class ( Fig. 1; Fig.…”

Section: Qpo's Originsupporting

confidence: 78%

“…Figs. 3 and 2 show that the QPO frequency is correlated with the disc temperature and with the flux of the total emission that is dominated by the disc (Neilsen et al 2011(Neilsen et al , 2012Mineo et al 2017), suggesting that the QPO is correlated with the disc. However, this does not mean that the QPO definitely originates from the disc.…”

Section: Qpo's Originmentioning

confidence: 94%

“…The disc and the corona are two essential spectral components for GRS 1915+105 during the ρ class (e.g. Neilsen et al 2011Neilsen et al , 2012Mineo et al 2012Mineo et al , 2017. Figs.…”

Section: Qpo's Originmentioning

confidence: 99%

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Disc–corona interaction in the heartbeat state of GRS 1915+105

Yan

Liu

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Timing analysis provides information about the dynamics of matter accreting on to neutron stars and black holes, and hence is crucial for studying the physics of the accretion flow around these objects. It is difficult, however, to associate the different variability components with each of the spectral components of the accretion flow. We apply several new methods to two Rossi X-ray Timing Explorer observations of the black hole binary GRS 1915+105 during its heartbeat state to explore the origin of the X-ray variability and the interactions of the accretion-flow components. We offer a promising window into the disc-corona interaction through analysing the formation regions of the disc aperiodic variabilities with different time-scales via comparing the corresponding transition energies of the amplitude-ratio spectra. In a previous paper, we analysed the Fourier power density as a function of energy and frequency to study the origin of the aperiodic variability, and combined that analysis with the phase lag as a function of frequency to derive a picture of the disc-corona interaction in this source. We here, for the first time, investigate the phase lag as a function of energy and frequency, and display some interesting details of the disc-corona interaction. Besides, the results from the shape of amplitude-ratio spectrum and from several other aspects suggest that the quasi-periodic oscillation originates from the corona.

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Section: Qpo's Originsupporting

confidence: 78%

Section: Qpo's Originmentioning

confidence: 94%

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Disc–corona interaction in the heartbeat state of GRS 1915+105

Yan

Liu

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…Several properties of this repeating bursting state of GRS 1915+105 were investigated in a series of papers Retired. (Massaro et al 2010;Mineo et al 2012Mineo et al , 2016Mineo et al , 2017Massa et al 2013) based on data series obtained in a long-duration study of this source with BeppoSAX in April 1999 and October 2000. According to the definition given in Mineo et al (2012) we distinguish in a burst the following three main segments: an initial increase of the photon count rate, the slow leading trail (SLT), up to the development of a pulse, frequently structured in a few narrow peaks, and terminating with a final decaying trail (FDT) to the initial level.…”

Section: Introductionmentioning

confidence: 99%

Energy scaling of the “heartbeat” pulse width of GRS 1915+105, IGR J17091−3624, and MXB 1730−335 from Rossi-XTE observations

Maselli

Capitanio

Feroci

et al. 2018

A&A

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We investigate some key aspects of the “heartbeat” variability consisting of series of bursts with a slow rise and a fast decay, thus far detected only in GRS 1915+105, IGR J17091−3624, and MXB 1730−335. A previous analysis based on BeppoSAX data of GRS 1915+105 revealed a hard-X delay (HXD), that is a lag of the burst rise at higher energies with respect to lower ones; this leads to narrower pulse widths, w, at higher energies. We here use some light curves of Rossi-XTE observations of GRS 1915+105 for a deeper analysis of this effect and search for its presence in those extracted from some IGR J17091−3624 and MXB 1730−335 observations performed with the same satellite. Our results show that, at variance with GRS 1915+105, no HXD is evident in the light curves of MXB 1730−335 and only a marginal HXD may be argued for IGR J17091−3624. For GRS 1915+105 we find a decreasing trend of the pulse width with energy following a power law w = A ⋅ E−s with an index s ≈ 0.8. Furthermore, we confirm the increase of the HXD with the recurrence time Trec of the bursts in each series that was already found in previous works using BeppoSAX data. Based on a spectral analysis of these three sources we conclude that the differences highlighted in the properties of the “heartbeat” variability are probably related to the different accreting compact object and the eventual presence of a corona in these binary interacting systems.

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“…We added to this model a low energy absorber and a high energy tail to represent a possible Comptonization component. Our previous analysis showed that the spectral emission of this source requires a hybrid Comptonization model (Mineo et al 2012(Mineo et al , 2017; however, the small PCA energy range we fitted (3.3-15 keV) does not allow for such a complex model. We then adopted the simple scattering component described by the XSPEC model Simpl (Steiner et al 2009) that takes any seed spectrum (the hot multi-temperature disk in our case) and scatters a fraction f sc of the photons into a power law with spectral index Γ.…”

Section: Spectral Analysismentioning

confidence: 83%

New analysis of the ρ-class bursts, known as the “heartbeat” of GRS 1915+105: Pulse profile and spectral properties

Mineo

Massa

Massaro

et al. 2021

A&A

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Context. We present the results of a new analysis of three long Rossi-XTE observations of the microquasar GRS 1915+105 in the ρ class, performed in 1997, 1999, and 2000, and characterized by different peak profiles. The first data set, labeled G-1, is dominated by a single peak, while in the third observation (G-3), all bursts show a clearly detectable couple of peaks. The second observation (G-2) shows an intermediate structure with a single peak and an emerging shoulder on the decay side. Aims. We devised a new procedure to obtain mean burst profiles in every energy channel independently of the recurrence time intervals of the bursts, variable from 45 s to 53 s in the considered observations, with the aim of investigating the different features of peaks and the eventual spectral variations. Methods. All the bursts were aligned at a common time bin on the decaying portion of the bursts that is stable in simultaneous light curves at different energies. An averaging algorithm was then applied without modifying the statistical properties or scaling the burst lengths. We analyzed the peak amplitude ratios and the dependence of their delays on energy. The spectral distributions were evaluated for the various components: a stable multi-temperature disk plus a power law Comptonization component was used for the baseline emission and temperature differences of peak components were evaluated with the inclusion of an additional blackbody. Results. In addition to the well-observed double peak (P1 and P2) pattern, we detected a third small peak (P3) in the structured G-3 light curve. This peak, differently from the other two, exhibits a fast rising and a slower exponential decay, with a e-folding time constant of 1.32 s. The blackbody temperatures of P2 and P3 are higher than P1 and the power law spectrum of P3 is the flattest one. Conclusions. The time and spectral behavior of P3 is interpreted as a signature of a relatively hot plasma outflow from the disk into the corona and its duration is consistent with the crossing timescale of the particles through the corona where electrons radiate.

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Comparing theρandχclass spectra of the microquasar GRS 1915+105 observed withBeppoSAX

Cited by 4 publications

References 48 publications

Disc–corona interaction in the heartbeat state of GRS 1915+105

Disc–corona interaction in the heartbeat state of GRS 1915+105

Energy scaling of the “heartbeat” pulse width of GRS 1915+105, IGR J17091−3624, and MXB 1730−335 from Rossi-XTE observations

New analysis of the ρ-class bursts, known as the “heartbeat” of GRS 1915+105: Pulse profile and spectral properties

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