Disk Tearing Leads to Low and High Frequency Quasi Periodic Oscillations in a GRMHD Simulation of a Thin Accretion Disk

Musoke, G.; Liska, M.; Porth, O.; van der Klis, M.; Ingram, A.

doi:10.48550/arxiv.2201.03085

Cited by 7 publications

(9 citation statements)

References 89 publications

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“…The results show that the Comptonization flux decreases when the disk tears, probably because the outer disc cannot maintain a sufficient gas supply (Liska et al 2021). Conversely, disk flux less than 2 keV increases slightly, which is also seen in recent simulations of Musoke et al (2022), although their main research is not type-B QPOs. They suggested that the absence of a warp in the aligned portion of the disk reduces the inflow speed of the gas, which increases the density.…”

Section: The Disappearances Of Type-b Qpossupporting

confidence: 75%

Transitions and Origin of the Type-B Quasi-Periodic Oscillation in the Black Hole X-ray Binary MAXI~ J1348--630

Liu¹,

Huang²,

Bu³

et al. 2022

Preprint

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The fast transitions between different types of quasi-periodic oscillations (QPOs) are generally observed in black hole transient sources (BHTs). We present a detailed study on the timing and spectral properties of the transitions of type-B QPOs in MAXI J1348-630, observed by Insight -HXMT. The fractional rms variability-energy relationship and energy spectra reveal that type-B QPOs probably originate from jet precession. Compared to weak power-law dominated power spectrum, when type-B QPO is present, the corresponding energy spectrum shows an increase in Comptonization component and the need for xillverCp component, and a slight increase of height of the corona when using relxilllp model. Therefore, we suggest that a coupled inner disk-jet region is responsible for the observed type-B QPOs transitions. The time scale for the appearance/disappearance of type-B QPOs is either long or short (seconds), which may indicate an instability of disk-jet structure. For these phenomena, we give the hypothesis that the Bardeen-Petterson effect causes disk-jet structure to align with BH spin axis, or that the disappearance of small-scale jets bound by the magnetic flux tubes lead to the disappearance of type-B QPOs. We observed three events regarding the B/C transitions, one of which occurred in a short time from ∼ 9.2 Hz (C) to ∼ 4.8 Hz (B). The energy spectral analysis for the other two transitions shows that when type-C QPO is present, the Comptonization flux is higher, the spectrum is harder and the inner radius of disk changes insignificantly. We suggest that type-C QPOs probably originate from relatively stronger jets or corona.

show abstract

Section: The Disappearances Of Type-b Qpossupporting

confidence: 75%

Transitions and Origin of the Type-B Quasi-Periodic Oscillation in the Black Hole X-ray Binary MAXI~ J1348--630

Liu¹,

Huang²,

Bu³

et al. 2022

Preprint

View full text Add to dashboard Cite

show abstract

“…(Liska et al 2021). Conversely, a disk flux less than 2 keV increases slightly, which is also seen in recent simulations of Musoke et al (2022), although their main research is not type-B QPOs. They suggested that the absence of a warp in the aligned portion of the disk reduces the inflow speed of the gas, which increases the density.…”

Section: The Disappearances Of Type-b Qpossupporting

confidence: 72%

Transitions and Origin of the Type-B Quasi-periodic Oscillations in the Black Hole X-Ray Binary MAXI J1348–630

Liu

Huang

Bu³

et al. 2022

ApJ

View full text Add to dashboard Cite

The fast transitions between different types of quasi-periodic oscillations (QPOs) are generally observed in black hole transient sources (BHTs). We present a detailed study of the timing and spectral properties of the transitions of type-B QPOs in MAXI J1348–630, observed by Insight-HXMT. The fractional rms variability–energy relationship and energy spectra reveal that type-B QPOs probably originate from jet precession. Compared to a weak power-law dominated power spectrum, when type-B QPOs are present, the corresponding energy spectrum shows an increase in the Comptonization component and the need for the xillverCp component, and a slight increase in the height of the corona when using the relxilllp model. Therefore, we suggest that a coupled inner disk-jet region is responsible for the observed type-B QPO transitions. The timescale for the appearance/disappearance of type-B QPOs is either long or short (seconds), which may indicate instability of the disk-jet structure. For these phenomena, we hypothesize that the Bardeen–Petterson effect causes the disk-jet structure to align with the BH spin axis or that the disappearance of small-scale jets bound by the magnetic flux tubes leads to the disappearance of type-B QPOs. We observed three events regarding the B/C transitions, one of which occurred over a short time period from ∼9.2 Hz (C) to ∼4.8 Hz (B). The energy spectral analysis for the other two transitions shows that when type-C QPO is present, the Comptonization flux is higher, the spectrum is harder, and the inner radius of the disk changes insignificantly. We suggest that type-C QPOs probably originate from relatively stronger jets or the corona.

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“…Liska et al (2019a) demonstrated, for the first time in GRMHD, that tilted thin magnetized disks align with the black hole midplane as theoretically predicted (Bardeen & Petterson 1975), solving a 40 yr old problem in astrophysical disk dynamics. Further, not only this article but also Liska et al (2021) and Musoke et al (2022) simulated disk tearing in highly tilted thin disks (Figure 3), potentially explaining some types of QPOs observed in XRBs (e.g., Kalamkar et al 2016), as well as holding important consequences for galactic evolution (e.g., King et al 2005). Using H-AMR, Chatterjee et al (2019) simulated the longest extent (in both temporal and spatial dimensions) relativistic jets from an accreting black hole in 2D GRMHD, making it possible to follow the jet over a range of 5 orders of magnitude in distance and enable the study of the jet's deceleration process as it carves out its path through the environment.…”

Section: Advancements In Computational Methodsmentioning

confidence: 88%

H-AMR: A New GPU-accelerated GRMHD Code for Exascale Computing with 3D Adaptive Mesh Refinement and Local Adaptive Time Stepping

Liska

Chatterjee

Danat

et al. 2022

ApJS

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General relativistic magnetohydrodynamic (GRMHD) simulations have revolutionized our understanding of black hole accretion. Here, we present a GPU-accelerated GRMHD code H-AMR with multifaceted optimizations that, collectively, accelerate computation by 2–5 orders of magnitude for a wide range of applications. First, it introduces a spherical grid with 3D adaptive mesh refinement that operates in each of the three dimensions independently. This allows us to circumvent the Courant condition near the polar singularity, which otherwise cripples high-resolution computational performance. Second, we demonstrate that local adaptive time stepping on a logarithmic spherical-polar grid accelerates computation by a factor of ≲10 compared to traditional hierarchical time-stepping approaches. Jointly, these unique features lead to an effective speed of ∼109 zone cycles per second per node on 5400 NVIDIA V100 GPUs (i.e., 900 nodes of the OLCF Summit supercomputer). We illustrate H-AMR's computational performance by presenting the first GRMHD simulation of a tilted thin accretion disk threaded by a toroidal magnetic field around a rapidly spinning black hole. With an effective resolution of 13,440 × 4608 × 8092 cells and a total of ≲22 billion cells and ∼0.65 × 108 time steps, it is among the largest astrophysical simulations ever performed. We find that frame dragging by the black hole tears up the disk into two independently precessing subdisks. The innermost subdisk rotation axis intermittently aligns with the black hole spin, demonstrating for the first time that such long-sought alignment is possible in the absence of large-scale poloidal magnetic fields.

show abstract

Disk Tearing Leads to Low and High Frequency Quasi Periodic Oscillations in a GRMHD Simulation of a Thin Accretion Disk

Cited by 7 publications

References 89 publications

Transitions and Origin of the Type-B Quasi-Periodic Oscillation in the Black Hole X-ray Binary MAXI~ J1348--630

Transitions and Origin of the Type-B Quasi-Periodic Oscillation in the Black Hole X-ray Binary MAXI~ J1348--630

Transitions and Origin of the Type-B Quasi-periodic Oscillations in the Black Hole X-Ray Binary MAXI J1348–630

H-AMR: A New GPU-accelerated GRMHD Code for Exascale Computing with 3D Adaptive Mesh Refinement and Local Adaptive Time Stepping

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