Deterministic Chaos in the X-ray Sources

Grzȩdzielski, Mikołaj; Suková, Petra; Janiuk, Agnieszka

doi:10.1007/s12036-015-9356-7

Cited by 7 publications

(6 citation statements)

References 15 publications

(14 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The recurrence analysis tool introduced by Eckmann et al (1987) and further developed by Marwan et al (2007) has been used in time series analysis of various experimental data sets for the purpose of distinguishing recurrent phenomena not easily extrapolated by other correlation methods. Recurrence analysis was recently used to characterise deterministic versus stochastic structure in the light curves of black hole X-ray binaries (Grzedzielski et al 2015, Suková et al 2016. The production of a recurrence plot (RP) is similar to the Close Returns method used in Sec.…”

Section: A3 Recurrence Analysismentioning

confidence: 99%

The chaotic long-term X-ray variability of 4U 1705–44

Phillipson

Boyd

Smale

2018

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

The low-mass X-ray binary 4U1705-44 exhibits dramatic long-term X-ray time variability with a timescale of several hundred days. The All-Sky Monitor (ASM) aboard the Rossi X-ray Timing Explorer (RXTE) and the Japanese Monitor of All-sky X-ray Image (MAXI) aboard the International Space Station together have continuously observed the source from December 1995 through May 2014. The combined ASM-MAXI data provide a continuous time series over fifty times the length of the timescale of interest. Topological analysis can help us identify 'fingerprints' in the phase-space of a system unique to its equations of motion. The Birman-Williams theorem postulates that if such fingerprints are the same between two systems, then their equations of motion must be closely related. The phase-space embedding of the source light curve shows a strong resemblance to the double-welled nonlinear Duffing oscillator. We explore a range of parameters for which the Duffing oscillator closely mirrors the time evolution of 4U1705-44. We extract low period, unstable periodic orbits from the 4U1705-44 and Duffing time series and compare their topological information. The Duffing and 4U1705-44 topological properties are identical, providing strong evidence that they share the same underlying template. This suggests that we can look to the Duffing equation to help guide the development of a physical model to describe the long-term X-ray variability of this and other similarly behaved X-ray binary systems.

show abstract

Section: A3 Recurrence Analysismentioning

confidence: 99%

The chaotic long-term X-ray variability of 4U 1705–44

Phillipson

Boyd

Smale

2018

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

show abstract

“…This increases the level of non-linearity in the equations, and most of the solutions with very small R out show complex multi-peak outbursts, characteristic of the first stage of the development of the deterministic chaos (see e.g. discussion by Grzedzielski et al 2015;Suková et al 2016, and the references therein). However, the details of this phenomenon are certainly sensitive to the way how this outer boundary is set, and this in principle should be related to the global scenario which allows us to consider the small value of R out as representing the reality.…”

Section: Discussionmentioning

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

View full text Add to dashboard Cite

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

“…Instabilities in the accretion discs are believed to be responsible for some observational features such as variabilities in the active galactic nuclei (AGNs) and the X-ray binaries (Janiuk & Czerny 2011;Dexter and Quataert 2012;Jiang et al 2013;Wu et al 2016), and the periodic X-ray variability of the Seyfert galaxies (Choi et al 2002;Czerny et al 2003;Kawaguchi 2003). The QPOs in BH discs are attributed to the viscous-thermal instability and the inertial-acoustic (pulsational) instability (e.g., Chen & Taam 1994, 1995Taam 1999;Dubus et al 2001;Fan et al 2008;Grzedzielski et al 2015). Although various types of the disc instabilities have been studied by many authors (e.g., Abramowicz et al 1984;Wu et al 1995a, b, c;Ding et al 2000;Khosravi & Khesali 2014, hereafter KK14), we briefly review the previous works related to the present study.…”

Section: Introductionmentioning

confidence: 99%

“…TI related to dwarf novae outburst was found by Hōshi (1979) and Meyer & Meyer-Hofmeister (1981). This instability in the discs around BHs or neutron stars is a promising mechanism to explain observed variabilities of X-ray binaries, galactic nuclei, and quasars (Shibazaki & Hōshi 1975;Shakura & Sanyave 1976;Kakubari et al 1989;Huang & Wheeler 1989;Choi et al 2002;Grzedzielski et al 2015). Radiationdominated inner region of a standard accretion disc is subject to TI and viscous instability (Lightman & Eardley 1974;Shakura & Sanyave 1976;Piran 1978;Blumentahal et al 1984;Wu et al 1995b;Wu & Li 1996, hereafter WL96;Dubus et al 2001;Kawanaka & Kohri 2012;Khesali & Khosravi 2013, hereafter KK13;Jiang et al 2013;Tessema 2014;Yu et al 2015).…”

Section: Introductionmentioning

confidence: 99%

The local stability of the magnetized advection-dominated discs with the radial viscous force

Ghoreyshi

Shadmehri

2018

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We study local stability of the advection-dominated optically thick (slim) and optically thin discs with purely toroidal magnetic field and the radial viscous force using a linear perturbation analysis. Our dispersion relation indicates that the presence of magnetic fields and radial viscous force cannot give rise to any new mode of the instability. We find, however, that growth rate of the thermal mode in the slim discs and that of the acoustic modes in the slim and optically thin discs are dramatically affected by the radial viscous force. This force tends to strongly decrease the growth rate of the outward-propagating acoustic mode (O-mode) at the short-wavelength limit, but it causes a slim disc to become thermally more unstable. We find that growth rate of the thermal mode increases in the presence of radial viscous force. This enhancement is more significant when the viscosity parameter is large. We also show that growth rate of the O-mode reduces when radial viscous force is considered. The growth rates of the thermal and acoustic modes depend on the magnetic field. Although the instability of O-mode for a stronger magnetic field case has a higher growth rate, the thermal mode of the slim discs can be suppressed when the magnetic field is strong. The inertialacoustic instability of a magnetized disc may explain the quasi-periodic oscillations (QPOs) from the black holes.

show abstract

Deterministic Chaos in the X-ray Sources

Abstract: Abstract. Hardly any of the observed black hole accretion disks in X-

Cited by 7 publications

References 15 publications

The chaotic long-term X-ray variability of 4U 1705–44

The chaotic long-term X-ray variability of 4U 1705–44

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

The local stability of the magnetized advection-dominated discs with the radial viscous force

Contact Info

Product

Resources

About