Bardeen‐Petterson Effect and Quasi‐periodic Oscillations in X‐Ray Binaries

Fragile, P. Chris; Mathews, Grant J.; Wilson, J. R.

doi:10.1086/320990

Cited by 73 publications

(80 citation statements)

References 49 publications

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“…The angular momentum, J, can be expressed in terms of the dimensionless spin parameter, a * , such that (Fragile et al 2001), and the precessional period (in days) becomes…”

Section: The Lense-thirring Effectmentioning

confidence: 99%

Feasibility study of Lense-Thirring precession in LS I +61°303

Massi

Zimmermann

2010

A&A

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Context. Very recent analysis of the radio spectral index and high energy observations have shown that the two-peak accretion/ejection microquasar model applies for LS I +61 • 303. Aims. The fast variations of the position angle observed with MERLIN and confirmed by consecutive VLBA images must therefore be explained in the context of the microquasar scenario. Methods.We calculate what could be the precessional period for the accretion disk in LS I +61 • 303 under tidal forces of the Be star (P tidal−forces ) or under the effect of frame dragging produced by the rotation of the compact object (P Lense−Thirring ). Results. P tidal−forces is more than one year. P Lense−Thirring depends on the truncated radius of the accretion disk, R tr . We determined R tr = 300r g for observed QPO at 2 Hz. This value is much above the few r g , where the Bardeen-Petterson effect should align the midplane of the disk. For this truncated radius of the accretion disk P Lense−Thirring for a slow rotator results in a few days. Conclusions. Lense-Thirring precession induced by a slowly rotating compact object could be compatible with the daily variations of the ejecta angle observed in LS I +61 • 303.

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“…The angular momentum, J, can be expressed in terms of the dimensionless spin parameter, a * , such that (Fragile et al 2001), and the precessional period (in days) becomes…”

Section: The Lense-thirring Effectmentioning

confidence: 99%

Feasibility study of Lense-Thirring precession in LS I +61°303

Massi

Zimmermann

2010

A&A

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“…NGC 3079 (Kondratko et al 2005), NGC 1068 (Caproni et al 2006), and NGC 4258 (Caproni et al 2007), may have accretion disks that are tilted with respect to the symmetry plane of their central black hole spacetimes. There are also compelling theoretical arguments that many black hole accretion disks should be tilted (Fragile et al 2001;Maccarone 2002). This applies to both stellar mass black holes, which can become tilted through asymmetric supernovae kicks (Fragos et al 2010) or binary captures and will remain tilted throughout their accretion histories, and to supermassive black holes in galactic centers, which will likely be tilted for some period of time after every major merger event (Kinney et al 2000).…”

Section: Tilted Disksmentioning

confidence: 99%

Current Status of Simulations

Fragile

2013

Space Sci Rev

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As the title suggests, the purpose of this chapter is to review the current status of numerical simulations of black hole accretion disks. This chapter focuses exclusively on global simulations of the accretion process within a few tens of gravitational radii of the black hole. Most of the simulations discussed are performed using general relativistic magnetohydrodynamic (MHD) schemes, although some mention is made of Newtonian radiation MHD simulations and smoothed particle hydrodynamics. The goal is to convey some of the exciting work that has been going on in the past few years and provide some speculation on future directions.

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“…(equatorial) flow [299,310,157], or waves in tilted discs resulting from the Bardeen-Peterson effect [113]. (Clearly, the processes can proceed in a symbiosis, for instance the secondary would probably actuate hot spots as well as oscillations in the disc, pulling some of its material out into a tilted orbit.)…”

Section: Galactic Nuclei and X-ray Binariesmentioning

confidence: 99%

Towards Gravitating Discs Around Stationary Black Holes

Semerák

2002

Gravitation: Following the Prague Inspiration

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This article outlines the search for an exact general relativistic description of the exterior (vacuum) gravitational field of a rotating spheroidal black hole surrounded by a realistic axially symmetric disc of matter. The problem of multi-body stationary spacetimes is first exposed from the perspective of the relativity theory (section 1) and astrophysics (section 2), listing the basic methods employed and results obtained. Then (in section 3) basic formulas for stationary axisymmetric solutions are summarized. Sections 4 and 5 review what we have learnt with MiroslavŽáček and Tomáš Zellerin about certain static and stationary situations recently. Concluding remarks are given in section 6. Although the survey part is quite general, the list of references cannot be complete. Our main desideratum was the informative value rather than originality -novelties have been preferred, mainly reviews and those with detailed introductions. The fields of multi-body systems involving black holesThe subject of self-gravitating sources around rotating black holes is interesting in several respects, relevant from the point of view of the relativity theory itself as well as in the astrophysical context.First, due to the non-linearity of Einstein's equations, the field of a multi-body system is a traditional challenge where one typically does not manage with a simple superposition. 1 On the first post-Newtonian level, the "celestial mechanics" of gravitationally interacting bodies can be kept linear [89,90], but in the strong-field region the interaction may bring surprising features that have only been described in a very few cases yet (for a two-body problem -today at the centre of attention because of the expected gravitational waves from colliding compact binaries, "the current state of art is the third post-Newtonian approximation" [91]).The second point in which the problem embodies the essence of general relativity is the effect of inertial frame dragging due to the rotation of the sources. Contrary to the Newtonian treatment which does not discriminate between static and stationary situation, the field is now determined not only by mass-energy configuration, but also by its motion within the bodies. The inertial space can be imagined as a viscous fluid mixed by the sources. In today's "gravitoelectromagnetic" language, gravity has not only an electric component, generated by the mass, but also a magnetic one, generated by mass currents; see [245, 103, 215, 298, 147, 79, 202, 201, 1 Even the problem of an "isolated" object is very difficult (mainly if its motion must be found as well, not mentioning the interior field) unless one makes some simple assumptions about its multipole structure; see e.g. [98,99,17] for a treatment of bodies with matter interior, [297] for that also valid for singular bodies such as black holes, and [40] for the case of point-like particles.

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Bardeen‐Petterson Effect and Quasi‐periodic Oscillations in X‐Ray Binaries

Cited by 73 publications

References 49 publications

Feasibility study of Lense-Thirring precession in LS I +61°303

Feasibility study of Lense-Thirring precession in LS I +61°303

Current Status of Simulations

Towards Gravitating Discs Around Stationary Black Holes

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