Features of the matter flows in the peculiar cataclysmic variable AE Aquarii

Isakova, P. B.; Ikhsanov, N. R.; Жилкин, А. Г.; Бисикало, Д. В.; Beskrovnaya, N. G.

doi:10.1134/s1063772916040065

Cited by 16 publications

(7 citation statements)

References 46 publications

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“…In addition, we can further calculate the GW amplitude by considering the upper limit values of the magnetic field strength, B dip . Thus, knowing that AE Aqr has B dip = 5.0 × 10 7 G (Isakova et al 2016), AR Sco has B dip = 5.0 × 10 8 G (Buckley et al 2017), and RX J0648 has B dip = 1.01 × 10 8 G (inferred by the magnetic dipole model), we use equation ( 11) to calculate the ellipticity of the star, and equation ( 12) to calculate the GW amplitude. In addition, we compute the gravitational luminosity from equation ( 13) and the efficiency of this process with respect to the spindown luminosity.…”

Section: Magnetic Deformationmentioning

confidence: 99%

Gravitational waves from fast-spinning white dwarfs

Sousa

Coelho

2020

Monthly Notices of the Royal Astronomical Society

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Two mechanisms of gravitational waves (GWs) emission in fast-spinning white dwarfs (WDs) are investigated: accretion of matter and magnetic deformation. In both cases, the GW emission is generated by an asymmetry around the rotation axis of the star. However, in the first case, the asymmetry is due to the amount of accreted matter on the magnetic poles, while in the second case it is due to the intense magnetic field. We have estimated the GW amplitude and luminosity for three binary systems that have a fast-spinning magnetized WD, namely, AE Aquarii, AR Scorpii and RX J0648.0-4418. We find that, for the first mechanism, the systems AE Aquarii and RX J0648.0-4418 can be observed by the space detectors BBO and DECIGO if they have an amount of accreted mass of δm ≥ 10 −5 M . For the second mechanism, the three systems studied require that the WD have a magnetic field above ∼ 10 9 G to emit GWs that can be detected by BBO. We also verified that, in both mechanisms, the gravitational luminosity has an irrelevant contribution to the spindown luminosity of these three systems. Therefore, other mechanisms of energy emission are needed to explain the spindown of these objects.

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Section: Magnetic Deformationmentioning

confidence: 99%

Gravitational waves from fast-spinning white dwarfs

Sousa

Coelho

2020

Monthly Notices of the Royal Astronomical Society

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“…Given the lack of such evidence, speedy magnetic propeller (Eracleous & Horne 1996; Wynn et al 1997) and ejector (Ikhsanov & Beskrovnaya 2012; Ikhsanov et al 2004) are supposed to operate in this star. Hydrodynamic calculations hint that the field does not hinder the formation of a transient disk (ring) surrounding the magnetosphere (Isakova et al 2016). AE Aqr also exhibits radio and millimeter synchrotron emission (e.g., Bastian et al 1988; Bookbinder & Lamb 1987).…”

Section: Introductionmentioning

confidence: 99%

The cataclysmic variable AE Aquarii: B–V color of the flares

et al. 2017

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We report simultaneous observations of the flaring behavior of the cataclysmic variable star AE Aquarii (AE Aqr). The observations are in Johnson B and V bands. The color-magnitude diagrams (B-V vs. V and B-V vs. B) show that the star becomes more blue as it becomes brighter. In our model, AE Aqr's behavior can be explained with flares (fireballs) with 0.03 ≤ B-V ≤ 0.30, and temperature in the interval 8000 ≤ T ≤ 12000. 1 How to cite this article: Zamanov RK, Latev GY, Boeva S, Ibryamov S, Nikolov GB, Stoyanov KA. The cataclysmic variable AE Aquarii: B-V color of the flares. Astron. Nachr. / AN. 2017;338:598-603.

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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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Features of the matter flows in the peculiar cataclysmic variable AE Aquarii

Cited by 16 publications

References 46 publications

Gravitational waves from fast-spinning white dwarfs

Gravitational waves from fast-spinning white dwarfs

The cataclysmic variable AE Aquarii: B–V color of the flares

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

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