Flow structure in magnetic close binary stars

Жилкин, А. Г.; Bisikalo, D. V.; Boyarchuk, A. A.

doi:10.3367/ufne.0182.201202a.0121

Cited by 41 publications

(39 citation statements)

References 61 publications

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“…The light curve of this system displays switching, drift of the poles, and even the simultaneous presence of several (three or four) regions of active accretion. Figure 7 presents the flow structure believed to be present in the BY Cam system, based on the results of three-dimensional computations [112,145]. This type of solution is fairly typical, and provides an impression of the main features of the flow structures present in the computations that have been carried out.…”

Section: Magnetic Cataclysmic Variablesmentioning

confidence: 99%

“…The clearest example is the AE Aqr system [158]. This may be because this system is located in a super-propeller state [112], when the magnetic white dwarf is rotating extremely rapidly. The influence of the magnetic field of the rapidly rotating white dwarf on the structure of the plasma flow in its Roche lobe is so great that, instead of an accretion disk, there is an intense outflow from the system.…”

Section: Magnetic Cataclysmic Variablesmentioning

confidence: 99%

“…Some of the matter at the outer boundary of the disk can leave the system through the vicinity of the Lagrange point L 3 , carrying away excess angular momentum and forming an intercomponent envelope (see, e.g., [108,109]). Gasdynamical processes occurring in the accretion disk and envelope lead to the formation of a complex flow pattern, including a whole series of stationary shocks, as well as a set of non-stationary and quasistationary elements contributing to the emission and absorption of the stellar radiation [110][111][112][113]. 16 BOYARCHUK et al…”

Section: 22mentioning

confidence: 99%

“…The flow structure in the Roche lobe of the accretor is very complex (Fig. 6), and can include the accretion disk; a flow of matter from the inner Lagrange point L 1 ; a circumdisk halo; an extended, stationary shock called a "hot line" that forms when the stream collides with the circumdisk halo; tidal shocks; the outgoing shock ahead of the disk; and a precessional wave in the disk [110][111][112][113]. The accretion disks make a substantial contribution to both the emission of the cataclysmic variable and to absorption during eclipse, with the peak of their blackbody radiation lying in the UV.…”

Section: 22mentioning

confidence: 99%

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Scientific problems addressed by the Spektr-UV space project (world space Observatory—Ultraviolet)

et al. 2016

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Abstract-The article presents a review of scientific problems and methods of ultraviolet astronomy, focusing on perspective scientific problems (directions) whose solution requires UV space observatories. These include reionization and the history of star formation in the Universe, searches for dark baryonic matter, physical and chemical processes in the interstellar medium and protoplanetary disks, the physics of accretion and outflows in astrophysical objects, from Active Galactic Nuclei to close binary stars, stellar activity (for both low-mass and high-mass stars), and processes occurring in the atmospheres of both planets in the solar system and exoplanets. Technological progress in UV astronomy achieved in recent years is also considered. The well advanced, international, Russian-led Spektr-UV (World Space Observatory-Ultraviolet) project is described in more detail. This project is directed at creating a major space observatory operational in the ultraviolet (115-310 nm). This observatory will provide an effective, and possibly the only, powerful means of observing in this spectral range over the next ten years, and will be an powerful tool for resolving many topical scientific problems.

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Section: Magnetic Cataclysmic Variablesmentioning

confidence: 99%

Section: Magnetic Cataclysmic Variablesmentioning

confidence: 99%

Section: 22mentioning

confidence: 99%

Section: 22mentioning

confidence: 99%

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Scientific problems addressed by the Spektr-UV space project (world space Observatory—Ultraviolet)

et al. 2016

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“…In the series of our papers [9][10][11][12][13][14][15] (see also the monograph [16]), we developed a 3D numerical model for mass transfer in semidetached binary systems taking into account the magnetic field of the accretor. The model assumes that the plasma dynamics are determined by the slow mean flow, against the background of that highspeed MHD waves propagate.…”

Section: Introductionmentioning

confidence: 99%

A numerical model for accretion in intermediate polars with dipolar magnetic fields

2015

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A three-dimensional numerical model for an accretion process investigation in the magnetosphere of a white dwarf in magnetic cataclysmic variables is developed. The model assumes that the white dwarf has a dipole magnetic field with its symmetry axis inclined to the rotation axis. The model is based on the equations of modified MHD, that describe the mean flow parameters in the wave MHD turbulence. Diffusion of the magnetic field and radiative heating and cooling are taken into account. The suitability of the model is confirmed by modeling the accretion in a typical intermediate polar. The computations show that a magnetosphere forms around the accretor, with the accretion occurring via columns. The accretion columns have a curtain-like shape, and arc-shaped zones of energy release form on the surface of the white dwarf in the magnetic poles area as a result of the matter infall.

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