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

Yan, Shu-Ping; Ji, Li; Liu, Siming; Méndez, Mariano; Wang, Na; Li, Xiangdong; Qu, J. L.; Sun, Wei; Ge, Ming-Yu; Liao, J. Y.; Niu, Shu; Ding, Guoqiang

doi:10.1093/mnras/stx2885

Cited by 8 publications

(3 citation statements)

References 85 publications

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“…thors found that the frequency of the QPO increases up to 3-4 keV and above that energy the frequency increases very slowly. A similar behaviour was observed in observations of some of the classes of GRS 1915+105 (Qu et al 2010;Yan et al 2012Yan et al , 2018.…”

Section: Energy Dependence Of the Fwhm Of 𝐿 𝑙supporting

confidence: 87%

“…There are other BH LMXBs in which the frequency of a component in the PDS changes with energy, namely GRS 1915+105 (Qu et al 2010;Yan et al 2012;van den Eĳnden et al 2017;Yan et al 2018), H 1743-322 (Li et al 2013van den Eĳnden et al 2017), XTE J1550-564 and XTE J1859+226 (van den Eĳnden et al 2017 and MAXI 1535-571 (Huang et al 2018). The behaviour of 𝐿 𝑙 is similar to the one observed for the QPO of MAXI J1535-571 with frequencies above 3 Hz presented in Huang et al (2018).…”

Section: Energy Dependence Of the Fwhm Of 𝐿 𝑙mentioning

confidence: 99%

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Variability and phase lags of the type-C quasi-periodic oscillation of MAXI J1348–630 with NICER

Alabarta

Méndez

García

et al. 2022

Monthly Notices of the Royal Astronomical Society

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We study the properties of the type-C quasi-periodic oscillation (type-C QPO) of MAXI J1348–630 during its 2019 outburst and reflare with NICER. This is the first time that the evolution of the properties of type-C QPOs are studied during an outburst reflare. We found that the properties of the type-C QPO during the reflare are similar to those of type-C QPOs observed in other black hole systems during outburst. This suggests that the physical processes responsible for type-C QPOs are the same in a reflare and in an outburst. We also found that the FWHM of a high-frequency broadband component observed during the reflare changes significantly with energy. We studied the energy-dependent fractional rms amplitude and phase lags of the type-C QPO from 0.5 keV to 12 keV. We found that the fractional rms amplitude increases up to 2–3 keV and then remains approximately constant above this energy, and the lag spectra of the type-C QPO are hard. We discuss the dependence of the fractional rms amplitude and phase lags with energy in the context of Comptonisation as the radiative mechanism driving the QPO rms and lag spectra.

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Section: Energy Dependence Of the Fwhm Of 𝐿 𝑙supporting

confidence: 87%

Section: Energy Dependence Of the Fwhm Of 𝐿 𝑙mentioning

confidence: 99%

Variability and phase lags of the type-C quasi-periodic oscillation of MAXI J1348–630 with NICER

Alabarta

Méndez

García

et al. 2022

Monthly Notices of the Royal Astronomical Society

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“…In this state, the source does not show much variability. It also spends a significant amount of time in a highly variable ρ class, also known as the heartbeat class (heartbeat class hereafter), which has been widely studied in the literature (Taam et al 1997;Paul et al 1998;Yadav et al 1999;Neilsen et al 2011Neilsen et al , 2012Pahari et al 2014;Yan et al 2018). The phase-resolved spectroscopy for the heartbeat class was done by Neilsen et al (2012) using RXTE/PCA data in 3.3-45.0 keV band.…”

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confidence: 99%

Time-resolved spectroscopy on the heartbeat state of GRS 1915+105 using AstroSat

Rawat,

Misra,

Jain

et al. 2022

Preprint

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AstroSat spectra of the black hole system GRS 1915+105 during the heartbeat state (with a varying oscillation period from 150 to 100 secs) were analysed using a truncated relativistic disc model along with a Comptonization component. Spectra were fitted for segments of length ∼ 24 secs. The oscillation can be described as coordinated variations of the accretion rate, Comptonised flux, and the inner disc radius, with the latter ranging from 1.235-5 gravitational radii. Comparison with results from the χ and Intermediate states shows that while the accretion rate and the high energy photon index were similar, the inner disc radius and the fraction of Comptonised photons were larger for these states than for the heartbeat one. The coronal efficiency η ≡ L ac / Ṁ c 2 , where L ac is the radiative luminosity generated in the corona is found to be approximately ∝ Ṁ −2/3 for all the observations. The efficiency decreases with inner radii for the heartbeat state but has similar values for the χ and Intermediate states where the inner radii is larger. The implications of these results are discussed.

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

Cited by 8 publications

References 85 publications

Variability and phase lags of the type-C quasi-periodic oscillation of MAXI J1348–630 with NICER

Variability and phase lags of the type-C quasi-periodic oscillation of MAXI J1348–630 with NICER

Time-resolved spectroscopy on the heartbeat state of GRS 1915+105 using AstroSat

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

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