Swift/XRT, Chandra, and XMM–Newton observations of IGR J17091–3624 as it returns into quiescence

Pereyra, Margarita; Altamirano, D.; Court, James; Degenaar, N.; Wijnands, Rudy; Parikh, A. S.; Cúneo, V. A.

doi:10.1093/mnras/staa2009

Cited by 6 publications

(3 citation statements)

References 64 publications

(77 reference statements)

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“…A similar so-called heartbeat variability of the microquasar IGR J17091 (RA: 01h19m08.68s Dec: −34d11m30.5s after NED 1 ) was discovered by Altamirano et al (2011), and its luminosity changes in X-ray band were also modeled by Janiuk et al (2015) by the accretion disk radiation pressure instability. However, this source recently returned to the quiescent state (Pereyra et al 2020). On the other hand, Bagnoli (2015) discovered heartbeat states in MXB 1730-335 (the Rapid Burster) that were later explored by Maselli et al (2018).…”

Section: Introductionmentioning

confidence: 99%

Modified models of radiation pressure instability applied to 10, 10⁵, and 10⁷ M_⊙ accreting black holes

Śniegowska

Grzȩdzielski

Czerny

et al. 2023

A&A

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Context. Some accreting black holes exhibit much stronger variability patterns than the usual stochastic variations. Radiation pressure instability is one of the proposed mechanisms that might account for this effect. Aims. We model luminosity changes for objects with a black hole mass of 10, 105, and 107 solar masses, using the time-dependent evolution of an accretion disk that is unstable as a result of the dominant radiation pressure. We concentrate on the outburst timescales. We explore the influence of the hot coronal flow above the cold disk, the inner purely hot flow, and the effect of the magnetic field on the time evolution of the disk-corona system. For intermediate-mass black holes and active galactic nuclei, we also explore the role of the disk outer radius because a disk that is fed by tidal disruption events (TDE) can be quite small. Methods. We used a 1D vertically integrated time-dependent numerical scheme that models the simultaneous evolution of the disk and corona, which is coupled by the vertical mass exchange. We parameterized the strength of the large-scale toroidal magnetic fields according to a local accretion rate. We also discuss a possible inner optically thin flow, the advection-dominated accretion flow (ADAF). This flow would require modification of the inner boundary condition of the cold disk flow. For the set of the global parameters, we calculated the variability timescales and outburst amplitudes of the disk and the corona. Results. We found that the role of the inner ADAF and the accreting corona are relatively unimportant, but the outburst character strongly depends on the magnetic field and on the outer radius of the disk if this radius is smaller (due to the TDE phenomenon) than the size of the instability zone in a stationary disk with infinite radius. For microquasars, the dependence on the magnetic field is monotonic, and the period decreases with the field strength. For higher black hole masses, the dependence is nonmonotonic, and an initial rise of the period is later replaced with a relatively rapid decrease as the magnetic field continues to rise. A still stronger magnetic field stabilizes the disk. When we assumed a smaller disk outer radiusfor 105 and 107 M⊙, the outbursts were shorter and led to complex multiscale outbursts for some parameters, thus approaching the behavior of deterministic chaos. Conclusions. Our computations confirm that the radiation pressure instability model can account for heartbeat states in microquasars. The rapid variability detected in intermediate-mass black holes in the form of quasi-periodic eruptions can be consistent with the model, but only when it is combined with the TDE phenomenon. The yearly repeating variability in changing-look active galactic nuclei in our model also requires a small outer radius either due to the recent TDE or due to the gap in the disk that is related to a secondary black hole.

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Section: Introductionmentioning

confidence: 99%

Modified models of radiation pressure instability applied to 10, 10⁵, and 10⁷ M_⊙ accreting black holes

Śniegowska

Grzȩdzielski

Czerny

et al. 2023

A&A

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show abstract

“…The long and bright outburst started in 2011 ended in 2013, with a return of the source to the LHS, a number of short reflares during the LHS, and a final descent into a very low- luminosity LHS, or a bright quiescence [376]. In 2016 February, IGR J17091−3624 showed another outburst, which, however, only lasted approximately 2 months with no sign of the heartbeat variability shown during the previous outburst [376].…”

Section: Igr J17091−3624mentioning

confidence: 98%

The INTEGRAL view on Black Hole X-ray Binaries

Motta,

Rodriguez,

Jourdain

et al. 2021

Preprint

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INTEGRAL is an ESA mission in fundamental astrophysics that was launched in October 2002. It has been in orbit for over 18 years, during which it has been observing the high-energy sky with a set of instruments specifically designed to probe the emission from hard X-ray and soft γ-ray sources. This paper is devoted to the subject of black hole binaries, which are among the most important sources that populate the high-energy sky. We present a review of the scientific literature based on INTEGRAL data, which has significantly advanced our knowledge in the field of relativistic astrophysics. We briefly summarise the state-of-the-art of the study of black hole binaries, with a particular focus on the topics closer to the INTEGRAL science. We then give an overview of the results obtained by INTEGRAL and by other observatories on a number of sources of importance in the field. Finally, we review the main results obtained over the past 18 years on all the black hole binaries that INTEGRAL has observed. We conclude with a summary of the main contributions of INTEGRAL to the field, and on the future perspectives.

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“…Similar 'heartbeat' variability of IGR J17091 microquasar (RA: 01h19m08.68s DEC: -34d11m30.5s after NED 1 ) was discovered by Altamirano et al (2011), and its luminosity changes in X-ray band have also been modeled by Janiuk et al (2015) by the accretion disk radiation pressure instability. However, recently this source returned to the quiescent state (Pereyra et al 2020). On the other hand, Bagnoli & in't Zand (2015) discovered the heartbeat states in MXB 1730-335 (the 'Rapid Burster'), later explored by Maselli et al (2018).…”

Section: Introductionmentioning

confidence: 99%

Modified models of radiation pressure instability in application to 10, 10$^5$, and 10$^7$ $M_{\odot}$ accreting black holes

Śniegowska¹,

Grzȩdzielski²,

Janiuk³

2022

Preprint

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Context. Some of the accreting black holes exhibit much stronger variability patterns than the usual stochastic variations. Radiation pressure instability is one of the proposed mechanisms which could account for this effect. Aims. We aim to model luminosity changes for objects with black hole mass of 10, 10 5 , and 10 7 solar masses, using the time-dependent evolution of an accretion disk unstable due to the dominant radiation pressure. We explore the influence of the hot coronal flow above the cold disk, the inner purely hot flow, and the effect of magnetic field on the time evolution of disk-corona system. In the case of Intermediate Mass Black Holes and AGN we also explore the role of the disk outer radius, motivated by the fact that the disk fed by Tidal Disruption Events can be quite small in size. Methods. We use a 1-dimensional, vertically integrated time-dependent numerical scheme which models simultaneous evolution of the disk and corona, coupled by the vertical mass exchange. We parameterize the strength of large-scale toroidal magnetic fields according to a local accretion rate. We also discuss the possibility of presence of an inner optically thin flow, namely the Advection-Dominated Accretion Flow (ADAF) which requires modification of the inner boundary condition of the cold disk flow. For the set of the global parameters we calculate the variability timescales and outburst amplitudes of the disk and the corona. Results. We found that the role of the inner ADAF and the accreting corona are relatively unimportant but the outburst character strongly depends on the magnetic field and the outer radius of the disk if this radius is smaller (due to TDE phenomenon) than the size of the instability zone in a stationary disk with infinite radius. For microquasars, the dependence on the magnetic field is monotonic, and the period decreases with the field strength. For larger black hole masses, the dependence is non-monotonic, and initial rise of the period is later replaced with the relatively rapid decrease as the magnetic field continues to rise. Still stronger magnetic field stabilizes the disk. Assumption of the smaller disk outer radius considered for 10 5 , and 10 7 M shortens the outbursts and for some parameter range leads to complex multi-scale outbursts thus approaching the deterministic chaos behaviour. Conclusions. Our computations confirm that the radiation pressure instability model can account for heartbeat states in microquasars. Rapid variability detected in IMBH in the form of Quasi-Periodic Ejection can be consistent with the model but only if combined with TDE phenomenon. Yearly repeating variability in Changing Look AGN also requires, in our model, small outer radius either due to the recent TDE or due to the presence of the gap in the disk related to the presence of a secondary black hole.

show abstract

Swift/XRT, Chandra, and XMM–Newton observations of IGR J17091–3624 as it returns into quiescence

Cited by 6 publications

References 64 publications

Modified models of radiation pressure instability applied to 10, 10⁵, and 10⁷ M_⊙ accreting black holes

Modified models of radiation pressure instability applied to 10, 10⁵, and 10⁷ M_⊙ accreting black holes

The INTEGRAL view on Black Hole X-ray Binaries

Modified models of radiation pressure instability in application to 10, 10$^5$, and 10$^7$ $M_{\odot}$ accreting black holes

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Swift/XRT, Chandra, and XMM–Newton observations of IGR J17091–3624 as it returns into quiescence

Cited by 6 publications

References 64 publications

Modified models of radiation pressure instability applied to 10, 105, and 107 M⊙ accreting black holes

Modified models of radiation pressure instability applied to 10, 105, and 107 M⊙ accreting black holes

The INTEGRAL view on Black Hole X-ray Binaries

Modified models of radiation pressure instability in application to 10, 10$^5$, and 10$^7$ $M_{\odot}$ accreting black holes

Contact Info

Product

Resources

About

Modified models of radiation pressure instability applied to 10, 10⁵, and 10⁷ M_⊙ accreting black holes

Modified models of radiation pressure instability applied to 10, 10⁵, and 10⁷ M_⊙ accreting black holes