Rossby wave instability and high-frequency quasi-periodic oscillations in accretion discs orbiting around black holes

Casse, Fabien; Vincent, F.

doi:10.1051/0004-6361/201935208

Cited by 5 publications

(6 citation statements)

References 45 publications

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“…While the precise method can be found in Varniere et al (2019), here we show in Fig. 5 a few examples of the PDSs made from our simulated light curves illustrating the ability of the RWI to produce a pair of peaks in the PDS that are similar to what has been observed.…”

Section: X-ray Light-curve and Power Density Spectrummentioning

confidence: 63%

“…Such an occurrence was first predicted by Tagger & Varniere (2006) and then explored further in Vincent et al (2013) but, in both cases, it was done using a pseudo-Newtonian approach for the purpose of mimicking the general relativistic effects upon the rotational velocity only. If we want to fully explore the behavior of the RWI around black holes, and especially its ability to explain fast variability (Varniere et al 2019), we therefore need to take into account all general relativistic effects upon both the fluid and its radiative emission.…”

Section: The Necessity For a Full General Relativistic Frameworkmentioning

confidence: 99%

“…2. This has led us, specifically in Varniere et al (2019), to study in more detail what causes the different modes to emerge. We found that the key component for which modes becomes dominant is the local condition of the system where the instability develops.…”

Section: X-ray Light-curve and Power Density Spectrummentioning

confidence: 99%

“…Across a series of recent papers (Casse et al 2017;Casse & Varniere 2018), we have studied how general relativity (GR) affects disc instabilities, such as the RWI, and found that except for high spin when the instability occurs inside 4r g , its behavior is similar to and well-approximated by its Newtonian equivalent. Furthermore, in Varniere et al (2019) we presented our Numerical Observatory of Violent Accreting systems (NOVAs) which is the perfect tool for performing the necessary direct comparison between the RWI "observable" and the X-ray data.…”

Section: Introductionmentioning

confidence: 99%

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Living on the edge: Rossby wave instability and HFQPOs in black hole binaries

Vincent

Casse

2020

A&A

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Context. The Rossby wave instability (RWI) has been proposed to explain the origin of the high-frequency quasi-periodic oscillations observed in the X-ray emission of astrophysical systems harbouring black holes. Recent numerical computations have proven that the RWI does exist in a general relativistic context and that its presence is associated with a time-variable X-ray emission from the disc. Aims. Using our new Numerical Observatory of Violent Accreting system, NOVAs, we explore the way the RWI impacts an accretion disc orbiting a spinning black hole under realistic astrophysical conditions. Our aim is to study the impact of the presence of the RWI in the very inner part of the accretion disc on known observables and explore some possibly new ones. Methods. We present the first full general relativistic hydrodynamical simulations of the RWI occurring at the last stable orbit of an accretion disc orbiting around a Kerr black-hole. Those simulations, coupled with a full general relativistic ray-tracing, have allowed us to directly compare our simulations with the observables we obtained from the X-ray emission of the disc. Results. Our study shows, for the first time, that the RWI naturally arises near the inner edge of an accretion disc whenever it gets close to its last stable orbit, as predicted analytically. From there, we show that not only does the RWI create a visible timing feature but it also impacts the energy spectrum of the source, which exhibits a high energy extension due to the presence of hot vortices generated by the RWI in the disc. Our study also shows that systems with the RWI present at the inner edge of the disc only exhibit similar behavior to systems in which HFQPOs have been detected.

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Section: X-ray Light-curve and Power Density Spectrummentioning

confidence: 63%

Section: The Necessity For a Full General Relativistic Frameworkmentioning

confidence: 99%

Section: X-ray Light-curve and Power Density Spectrummentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Living on the edge: Rossby wave instability and HFQPOs in black hole binaries

Vincent

Casse

2020

A&A

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“…Another explanation of HFQPOs is based on the Keplerian and radial frequencies of the deformation of the clumps of matter due to the simulated tidal interactions in the accretion disk (Germanà et al 2009). A recent model involves the study of (magneto)hydrodynamic instabilities, for example, in particular, to understand the 3:2 resonance of HFQPOs using the general relativistic and ray-tracing simulations (Tagger & Varnière 2006;Varniere et al 2019).…”

Section: Introductionmentioning

confidence: 99%

A geometric origin for quasi-periodic oscillations in black hole X-ray binaries

Rana,

Mangalam

2020

Preprint

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We expand the Relativistic Precession Model (RPM) to include non-equatorial and eccentric trajectories and apply it to Quasi-periodic oscillations (QPOs) in black hole Xray binaries (BHXRB) and associate their frequencies with the fundamental frequencies of the general case of non-equatorial (with Carter's constant, Q = 0) and eccentric (e = 0) particle trajectories, around a Kerr black hole. We study cases with either two or three simultaneous QPOs and extract the parameters {e, r p , a, Q}, where r p is the periastron distance of the orbit, and a is the spin of the black hole. We find that the orbits with [Q = 0 − 4] should have e 0.5 and r p ∼ 2 − 20 for the observed range of QPO frequencies, where a ∈ [0, 1], and that the spherical trajectories {e = 0, Q = 0} with Q = 2 − 4 should have r s ∼ 3 − 20. We find non-equatorial eccentric solutions for both M82 X-1 and GROJ 1655-40. We see that these trajectories, when taken together, span a torus region and give rise to a strong QPO signal. For two simultaneous QPO cases, we found equatorial eccentric orbit solutions for XTEJ 1550-564, 4U 1630-47, and GRS 1915+105, and spherical orbit solutions for BHXRB M82 X-1 and XTEJ 1550-564. We also show that the eccentric orbit solution fits the PBK correlation observed in BHXRB GROJ 1655-40. Our analysis of the fluid flow in the relativistic disk edge suggests that instabilities cause QPOs to originate in the torus region. We also present some useful formulae for trajectories and frequencies of spherical and equatorial eccentric orbits.

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Impact of a binary black hole on its outer circumbinary disc

Mignon-Risse¹,

Casse²

2022

Monthly Notices of the Royal Astronomical Society

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Accreting supermassive binary black holes (SMBBHs) are potential targets for multi-messenger astronomy as they emit gravitational waves (GW) while their environment emits electromagnetic (EM) waves. In order to get the most out of a joint GW-EM detection we first need to obtain theoretically-predicted EM signals unambiguously linked to BBHs. In that respect, this is the first of a series of papers dedicated to accreting pre-merger BBHs and their associated EM observables. Here, we extend our Numerical Observatory of Violent Accreting systems, e-NOVAs, to any spacetime. Unlike previous studies, almost exclusively focused on the inner regions, we investigated the impact of the BBH on its outer circumbinary disc, located in the radiation (or wave) zone, after implementing an approximate analytical spacetime of spinning, inspiralling BBHs in e-NOVAs. We follow the formation of a weak spiral structure in disc density arising from the retardation effects in the radiation zone metric. Simulation data are then post-processed with a general-relativistic ray-tracing code incorporating the same BBH spacetime, assuming SMBBH sources. The density spiral creates a small $({<}1\%)$ but unambiguous modulation of the lightcurve at the semi-orbital period. This signal, although weak, is fundamentally different from that of an axisymmetric disc around a single BH providing a lower limit on the impact of a BBH on its outer disc. This potential difference being found, we study how binary parameters impact this modulation in order to find the optimal case which is a high source inclination of any binary mass ratio (from 0.1 to 1).

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Rossby wave instability and high-frequency quasi-periodic oscillations in accretion discs orbiting around black holes

Cited by 5 publications

References 45 publications

Living on the edge: Rossby wave instability and HFQPOs in black hole binaries

Living on the edge: Rossby wave instability and HFQPOs in black hole binaries

A geometric origin for quasi-periodic oscillations in black hole X-ray binaries

Impact of a binary black hole on its outer circumbinary disc

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