Features of the accretion in the EX Hydrae system: Results of numerical simulation

Isakova, P. B.; Жилкин, А. Г.; Бисикало, Д. В.; Семена, А. Н.; Revnivtsev, M.

doi:10.1134/s1063772917070022

Cited by 11 publications

(5 citation statements)

References 32 publications

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“…Figure 1 demonstrates the full pattern of the material flow from the donor surface. The computational 1 Estimates of the influence of the plasma conductivity on the field line velocity carried out in our recent study [35] demonstrate that this effect is less than 20% in the accretion disk. This effect should apparently be even less important in the accretion streams of polars.…”

Section: Computational Resultsmentioning

confidence: 89%

“…Estimates of the influence of the plasma conductivity on the field line velocity carried out in our recent study[35] demonstrate that this effect is less than 20% in the accretion disk. This effect should apparently be even less important in the accretion streams of polars.2 State registration number 2016663823.…”

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confidence: 79%

“…To describe the slow proper motion of the plasma, it is necessary to distinguish the rapidly propagating fluctuations and apply a specific procedure for the ensemble averaging of the wave pulsations. We developed this model for MHD flows in application to polars and intermediate polars in [29,30,31,32,33,34,35].…”

Section: Formulation Of the Problemmentioning

confidence: 99%

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Features of the Flow Structure in the Vicinity of the Inner Lagrangian Point in Polars

2018

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The structures of plasma flows in close binary systems whose accretors have strong intrinsic magnetic fields are studied. A close binary system with the parameters of a typical polar is considered. The results of three dimensional numerical simulations of the material flow from the donor into the accretor Roche lobe are presented. Special attention is given to the flow structure in the vicinity of the inner Lagrangian point, where the accretion flow is formed. The interaction of the accretion flow material from the envelope of the donor with the magnetic field of the accretor results in the formation of a hierarchical structure of the magnetosphere, because less dense areas of the accretion flow are captured by the magnetic field of the white dwarf earlier than more dense regions. Taking into account this kind of magnetosphere structure can affect analysis results and interpretation of the observations. * isakovapb@inasan.ru

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Section: Computational Resultsmentioning

confidence: 89%

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confidence: 79%

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Features of the Flow Structure in the Vicinity of the Inner Lagrangian Point in Polars

2018

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“…This model is based on the equations system of modified magnetic hydrodynamics, which describes astrophysical flows under conditions of a strong external magnetic field. We have successfully applied this approach to modeling the flow structure for both polars and intermediate polars [5,[16][17][18][19][20][21][22][23][24][25][26][27][28].…”

Section: Numerical Modelmentioning

confidence: 99%

Hot Spots Drift in Synchronous and Asynchronous Polars: Results of Three-Dimensional Numerical Simulation

2021

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In this paper, the characteristics of hot spots on an accretor surface are investigated for two types of polars: the eclipsing synchronous polar V808 Aur and the non-eclipsing asynchronous polar CD Ind in configuration of an offset and non-offset magnetic dipole. The drift of hot spots is analyzed based on the results of numerical calculations and maps of the temperature distribution over the accretor surface. It is shown that a noticeable displacement of the spots is determined by the ratio of ballistic and magnetic parts of the jet trajectory. In the synchronous polar, the dominant influence on the drift of hot spots is exerted by variations in the mass transfer rate, which entail a change in the ballistic part of the trajectory. It was found that when the mass transfer rate changes within the range of 10−10M⊙/year to 10−7M⊙/year, the displacement of the hot spot in latitude and longitude can reach 30∘. In the asynchronous polar, a change in the position of hot spots is mainly defined by the properties of the white dwarf magnetosphere, and the displacement of hot spots in latitude and longitude can reach 20∘.

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“…There is also a population of cataclysmic variables where approximately 25% of the WDs are magnetic (Ferrario et al 2015). It has long been known that a magnetic field on a WD (or other accreting body) can have a dramatic effect on accretion dynamics (e.g : Cropper 1990;Collier Cameron and Campbell 1993;King 1993;Wynn and King 1995;Schmidt et al 1999;Li and Wilson 1999;Wu 2000;Alecian et al 2007;Bouvier et al 2007;Gregory and Donati 2011;Zhilkin et al 2012;Hussain and Alecian 2014;Wickramasinghe 2014;Isakova et al 2017;Van Box Som et al 2018;Ablimit and Maeda 2019;Shahbaz 2019). Farihi et al (2017) use a model where dust is trapped in the magnetosphere of a WD to explain the observational anomaly in WD1145+017.…”

Section: Introductionmentioning

confidence: 99%

The Effect of a Magnetic Field on the Dynamics of Debris Discs Around White Dwarfs

Hogg,

Cutter,

Wynn

2020

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Observational estimates of the lifetimes and inferred accretion rates from debris discs around polluted white dwarfs are often inconsistent with the predictions of models of shielded Poynting-Robertson drag on the dust particles in the discs. Moreover, many cool polluted white dwarfs do not show any observational evidence of accompanying discs. This may be explained, in part, if the debris discs had shorter lifetimes and higher accretion rates than predicted by Poynting-Robertson drag alone. We consider the role of a magnetic field on tidally disrupted diamagnetic debris and its subsequent effect on the formation, evolution, and accretion rate of a debris disc. We estimate that magnetic field strengths greater than ∼10kG may decrease the time needed for circularisation and the disc lifetimes by several orders of magnitude and increase the associated accretion rates by a similar factor, relative to Poynting-Robertson drag. We suggest some polluted white dwarfs may host magnetic fields below the typical detectable limit and that these fields may account for a proportion of polluted white dwarfs with missing debris discs. We also suggest that diamagnetic drag may account for the higher accretion rate estimates among polluted white dwarfs that cannot be predicted solely by Poynting-Robertson drag and find a dependence on magnetic field strength, orbital pericentre distance, and particle size on predicated disc lifetimes and accretion rates.

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Features of the accretion in the EX Hydrae system: Results of numerical simulation

Cited by 11 publications

References 32 publications

Features of the Flow Structure in the Vicinity of the Inner Lagrangian Point in Polars

Features of the Flow Structure in the Vicinity of the Inner Lagrangian Point in Polars

Hot Spots Drift in Synchronous and Asynchronous Polars: Results of Three-Dimensional Numerical Simulation

The Effect of a Magnetic Field on the Dynamics of Debris Discs Around White Dwarfs

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