Excitation of turbulence in accretion disks of binary stars by non-linear perturbations

Kurbatov, E. P.; Бисикало, Д. В.

doi:10.1134/s1063772917060075

Cited by 5 publications

(3 citation statements)

References 25 publications

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“…The broad-band variability is often attributed to (i) inward propagating fluctuations driven by stochastic variability in the angular momentum transport mechanism (Lyubarskii 1997); (ii) turbulence, vortexes in the disc (e.g. Dobrotka et al 2010;Kurbatov & Bisikalo 2017); (iii) spiral structures in the disc (e.g. Baptista & Bortoletto 2008).…”

Section: Temperature In the Accretion Discmentioning

confidence: 99%

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Flickering of the jet‐ejecting symbiotic star MWC 560

et al. 2020

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We analyse optical photometric data of short term variability (flickering) of the accreting white dwarf in the jet-ejecting symbiotic star MWC 560. The observations are obtained in 17 nights during the period November 2011 -October 2019. The colour-magnitude diagram shows that the hot component of the system becomes redder as it gets brighter. For the flickering source we find that it has colour 0.14 < B − V < 0.40, temperature in the range 6300 < T f l < 11000 K, and radius 1.2 < R f l < 18 R ⊙ . We find a strong correlation (correlation coefficient 0.76, significance < 0.001) between B band magnitude and the average radius of the flickering source -as the brightness of the system increases the size of the flickering source also increases. The estimated temperature is similar to that of the bright spot of cataclysmic variables. In 2019 the flickering is missing, and the B-V colour of the hot component becomes bluer.

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Section: Temperature In the Accretion Discmentioning

confidence: 99%

“…; (ii) turbulence, vortexes in the disc (e.g Dobrotka et al 2010;Kurbatov & Bisikalo 2017)Baptista & Bortoletto 2008)…”

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confidence: 99%

Flickering of the jet‐ejecting symbiotic star MWC 560

et al. 2020

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“…Distribution of the angular momentum along the disk is close to Keplerian. At this, contribution of the gas pressure and radial component of the kinetic energy to the radial balance of forces is small (of the order of the square of the ratio of the disk thickness to radial scale [27,28]). However, one can not neglect the thermal structure of the disk, which determines intensity of the shock wave and is important for evaluation of the response of the disk to the loss of mass by accretor.…”

Section: Formulation Of the Problemmentioning

confidence: 99%

Possible Electromagnetic Manifestations of Merging Black Holes

2019

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We consider scenario of merger of two stellar mass black holes surrounded by an accretion disk. Due to emission of gravitational waves, the mass of the central object decreases and accretion disk experiences perturbation. Calculations show that the main consequence of this disturbance is formation of a shock wave propagating from the center of the disk to its periphery. Light curve is computed and duration of the flash is estimated under assumption that the flash terminates when the luminosity returns to the initial value.It is shown that, if the total mass of the merging binary is 55 M ⊙ (like in the event GW170814), the flash produced by the shock will increase bolometric luminosity of the disk by 4 6 orders of magnitude, up to 10 45 erg/s (absolute stellar magnitude −23.8 m ). With account of the distance to the source (540 Mpc) and for reasonable assumptions on the parameters of the accretion disk, it turns out that the apparent magnitude of the flash at the maximum of the spectral flux density should be 12.8 m 14.2 m , while duration of the flash few minutes.The main part of the shock radiation flux is emitted in the X-ray and gamma-ray ranges. In the spectral band of the EPIC instrument of the XMM-Newton observatory or the telescope eROSITA of the Spectrum-RG observatory (0.3 10 keV), luminosity will increase by 3 4 orders of magnitude (7.5 m 10 m ), up to 10 44 erg/s, corresponding to the apparent stellar magnitude about 17 m . Luminosity is at maximum in the observational band of the IBIS instrument of the INTEGRAL observatory (20 keV 10 MeV) and will be 10 44 10 45 erg/s, corresponding to the apparent flux 10 −4 photons per /cm 2 /s/keV at the wavelength ∼ 100 keV. From the far UV to the longer wavelengths, the brightening is virtually absent at the wavelength 10 eV luminosity, approximately, doubles and corresponds to the absolute magnitude −6 m and visual one 32 m . * bisikalo@inasan.ru † zhilkin@inasan.ru ‡ kurbatov@inasan.ru Object M 1 , M 2 [M ⊙ ] ∆M/(M 1 + M 2 ) [%] D [Mpc] GW150914 [1] 36 +5 −4 , 29 +4 −4 3.3 5.2 410 +160 −180 GW151226 [2] 14.2 +8.3 −3.7 , 7.5 +2.3 −2.3 2.9 5.5 440 +180 −190 GW170104 [3] 31.2 +8.4 −6.0 , 19.4 +8.3 −5.9 2.3 5.7 880 +450 −390 GW170608 [4] 12 +7 −2 , 7 +2 −2 2.8 5.1 340 +140 −140 GW170814 [5] 30.5 +5.7 −3.0 , 25.3 +2.8 −4.2 4.0 5.8 540 +130 −210

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The role of atmospheric outflows in the migration of hot Jupiters

Kurbatov

Бисикало

2021

Monthly Notices of the Royal Astronomical Society

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Many of observed hot Jupiters are subject to atmospheric outflows. Numerical simulations have shown that the matter escaping from the atmosphere can accumulate outside the orbit of the planet, forming a torus. In a few 108 yr, the mass of the torus can become large enough to exert a significant gravitational effect on the planet. Accumulation of mass, in its own turn, is hindered by the activity of the star, which leads to the photoevaporation of the torus matter. We explore the role of these and other factors in the planet’s migration in the epoch when the protoplanetary disk has already disappeared. Using HD 209458 system as an example, we show that the gravitational interaction with the torus leads to the possibility of migration of the planet to its observable position, starting from an orbit ≳ 0.3 AU.

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Excitation of turbulence in accretion disks of binary stars by non-linear perturbations

Cited by 5 publications

References 25 publications

Flickering of the jet‐ejecting symbiotic star MWC 560

Flickering of the jet‐ejecting symbiotic star MWC 560

Possible Electromagnetic Manifestations of Merging Black Holes

The role of atmospheric outflows in the migration of hot Jupiters

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