StingraySoftware/stingray: Version 0.3

Bachetti, Matteo; Huppenkothen, Daniela; Khan, Usman A.; Mishra, Himanshu; Sharma, Swapnil; Stevens, Abbie; Desai, Amogh; Rashid, Haroon; Ribeiro, Evandro M.; Swinbank, J.; Sipőcz, Brigitta; tappina,; omargamal,; Davis, Meg; Rasquinha, Achilles; Balm, P.H.M.; Mumford, Stuart; Campana, R.; Garg, Nitish; Tandon, Akash; Hota, Anurag; Nick,; Raj, Rashmi; Mishra, Sashank; Smith, Arfon M.; Mahlke, Max; Sachidanand, Saurav; Kumar, Sandeep; Blanco, Ricardo Vallés; Kothari, Sambhav

doi:10.5281/zenodo.4881255

Cited by 5 publications

(2 citation statements)

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“…This work has utilised the Stingray Python library for spectral timing: DOI: 10.5281/zenodo.4881255 (Bachetti et al 2021), LM-FIT: Non-Linear Least-Square Minimization and Curve-Fitting for Python package DOI: 10.5281/zenodo.11813, NumPy (Harris et al 2020), Matplotlib (Hunter 2007) and SciPy (Virtanen et al 2020).…”

Section: Acknowledgementsmentioning

confidence: 99%

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

Musoke,

Liska,

Porth

et al. 2022

Preprint

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Black hole X-ray binaries (BHXRBs) display a wide range of variability phenomena, from long duration spectral state changes to short-term broadband variability and quasi-periodic oscillations (QPOs). A particularly puzzling aspect is the production of QPOs, which -if properly understood -could be used as a powerful diagnostic tool of black hole accretion and evolution. In this work we analyse a high resolution three-dimensional general relativistic magnetohydrodynamic simulation of a geometrically thin accretion disk which is tilted by 65 • with respect to the black hole spin axis. We find that the Lense-Thirring torque from the rapidly spinning 10 𝑀 black hole causes several sub-disks to tear off within ∼ 10 − 20 gravitational radii. Tearing occurs in cycles on timescales of seconds. During each tearing cycle the inner sub-disk precesses for 1-5 periods before it falls into the black hole. We find a precession frequency of ∼ 3Hz, consistent with observed low-frequency QPOs. In addition, we find a high frequency QPO (HFQPO) with centroid frequency of ∼ 55Hz in the power spectra of the mass-weighted radius of the inner disk. This signal is caused by radial epicyclic oscillations of a dense ring of gas at the tearing radius, which strongly suggests a corresponding modulation of the X-ray lightcurve and may thus explain some of the observed HFQPOs.

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Section: Acknowledgementsmentioning

confidence: 99%

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

Musoke,

Liska,

Porth

et al. 2022

Preprint

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show abstract

“…Finally, after determining the most significant QPO frequencies at different times within each observation, we folded the light curves on those frequencies and obtained their phaseograms. We did that with the (Huppenkothen et al 2019a;Huppenkothen et al 2019b;Bachetti et al 2021) Python package, designed for spectraltiming analysis of X-ray data.…”

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confidence: 99%

Quasi periodic whispers from a transient ULX in M\,101: signatures of a fast-spinning neutron star?

Urquhart,

Soria,

Di Stefano

et al. 2022

Preprint

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We have studied the unusual time variability of an ultraluminous X-ray source in M 101, 4XMM J140314.2+541806 (henceforth, J1403), using Chandra and XMM-Newton data. Over the last two decades, J1403 has shown short-duration outbursts with an X-ray luminosity ∼1-3 ×10 39 erg s −1 , and longer intervals at luminosities ∼0.5-1 ×10 38 erg s −1 . The bimodal behaviour and fast outburst evolution (sometimes only a few days) are more consistent with an accretor/propeller scenario for a neutron star than with the canonical outburst cycles of stellar-mass black holes. If this scenario is correct, the luminosities in the accretor and propeller states suggest a fast spin (𝑃 ≈ 5 ms) and a low surface magnetic field (𝐵 ∼ 10 10 G), despite our identification of J1403 as a high-mass X-ray binary. The most striking property of J1403 is the presence of strong ∼600-s quasi periodic oscillations (QPOs), mostly around frequencies of ≈1.3-1.8 mHz, found at several epochs during the ultraluminous regime. We illustrate the properties of such QPOs, in particular their frequency and amplitude changes between and within observations, with a variety of techniques (Fast Fourier Transforms, Lomb-Scargle periodograms, weighted wavelet Z-transform analysis). The QPO frequency range <10 mHz is an almost unexplored regime in X-ray binaries and ultraluminous X-ray sources. We compare our findings with the (few) examples of very low frequency variability found in other accreting sources, and discuss possible explanations (Lense-Thirring precession of the inner flow or outflow; radiation pressure limit-cycle instability; marginally stable He burning on the neutron star surface).

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Quasi-periodic whispers from a transient ULX in M 101: signatures of a fast-spinning neutron star?

Urquhart

Soria

Stefano

et al. 2022

Monthly Notices of the Royal Astronomical Society

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We have studied the unusual time variability of an ultraluminous X-ray source in M 101, 4XMM J140314.2+541806 (henceforth, J1403), using Chandra and XMM-Newton data. Over the last two decades, J1403 has shown short-duration outbursts with an X-ray luminosity ∼1–3 × 1039 erg s−1, and longer intervals at luminosities ∼0.5–1 × 1038 erg s−1. The bimodal behaviour and fast outburst evolution (sometimes only a few days) are more consistent with an accretor/propeller scenario for a neutron star than with the canonical outburst cycles of stellar-mass black holes. If this scenario is correct, the luminosities in the accretor and propeller states suggest a fast spin (P ≈ 5 ms) and a low surface magnetic field (B ∼ 1010 G), despite our identification of J1403 as a high-mass X-ray binary. The most striking property of J1403 is the presence of strong ∼600-s quasi periodic oscillations (QPOs), mostly around frequencies of ≈1.3–1.8 mHz, found at several epochs during the ultraluminous regime. We illustrate the properties of such QPOs, in particular their frequency and amplitude changes between and within observations, with a variety of techniques (Fast Fourier Transforms, Lomb-Scargle periodograms, weighted wavelet Z-transform analysis). The QPO frequency range <10 mHz is an almost unexplored regime in X-ray binaries and ultraluminous X-ray sources. We compare our findings with the (few) examples of very low frequency variability found in other accreting sources, and discuss possible explanations (Lense-Thirring precession of the inner flow or outflow; radiation pressure limit-cycle instability; marginally stable He burning on the neutron star surface).

show abstract

StingraySoftware/stingray: Version 0.3

Cited by 5 publications

References 0 publications

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

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

Quasi periodic whispers from a transient ULX in M\,101: signatures of a fast-spinning neutron star?

Quasi-periodic whispers from a transient ULX in M 101: signatures of a fast-spinning neutron star?

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