Structure of the circumbinary envelope around a young binary system

Kaigorodov, P. V.; Bisikalo, D. V.; Fateeva, A. M.; Sytov, A. Yu.

doi:10.1134/s1063772910120024

Cited by 31 publications

(32 citation statements)

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“…The flow of matter in binary systems accreting material from protoplanetary disks has been simulated numerically in many studies [7][8][9][10][11][12][13][14][15][16][17]. The simulation results indicate the following major flow elements in these systems: circumstellar accretion disks around the system components, a rarefied area in the central parts of the protoplanetary disk adjoining the binary, and a complex system of gas-dynamical flows.…”

Section: Introductionmentioning

confidence: 99%

“…For reverse rotation to occur, the angular momentum delivered to the disk by the falling matter must be opposite to the angular momentum of the system. Numerical simulations of these systems have been performed in various studies [7][8][9][10][11][12][13][14][15][16][17], have not indicated the appearance of reversed accretion disks in binary systems for a wide range of parameters. In addition, analysis of the flow structure that forms in the vicinity of a young binary indicates that flows directed opposite to the motion of the components can exist [15].…”

Section: A Model For the Formation Of A Reversed Accretion Diskmentioning

confidence: 99%

“…The simulation results indicate the following major flow elements in these systems: circumstellar accretion disks around the system components, a rarefied area in the central parts of the protoplanetary disk adjoining the binary, and a complex system of gas-dynamical flows. The analysis of calculation results [14][15][16] indicate that the supersonic orbital motion of the system components through the gas of the protoplanetary disk leads to bow shocks formation ahead of the circumstellar accretion disk of each component; these bow shocks predominantly determine the dynamics of the matter in the area of decreased density in the central part of the protoplanetary disk, as well as accretion processes in the system. The results of numerical simulations agree well with the observed flow morphologies for systems whose inner structure is resolved.…”

Section: Introductionmentioning

confidence: 99%

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Reverse rotation of the accretion disk in RW Aur A: Observations and a physical model

et al. 2012

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Speckle interferometry of the young binary system RW Aur was performed with the 6-m telescope of the Special Astrophysical Observatory of the Russian Academy of Sciences using filters with central wavelengths of 550 nm and 800 nm and passband halfwidths of 20 nm and 100 nm, respectively. The angular separation of the binary components was 1.448 ′′ ± 0.005 and the position angle of the system was 255.9 o ± 0.3. at the observation epoch (JD 2 454 255.9). We find using published data that these values have been changing with mean rates of +0.002 ′′ /yr and +0.02 o /yr, respectively, over the past 70 years. This implies that the direction of the orbital motion of the binary system is opposite to the direction of the disk rotation in RW Aur A. We propose a physical model to explain the formation of circumstellar accretion disks rotating in the reverse direction relative to young binary stars surrounded by protoplanetary disks. Our model can explain the characteristic features of the matter flow in RW Aur A: the high accretion rate, small size of the disk around the massive component, and reverse direction of rotation.

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Section: Introductionmentioning

confidence: 99%

Section: A Model For the Formation Of A Reversed Accretion Diskmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Reverse rotation of the accretion disk in RW Aur A: Observations and a physical model

et al. 2012

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“…They come in two flavors: First, the systems where at least one component of the binary hosts a circumstellar disks, as studied by Regály et al (2011a,b); and second, binaries with a circumbinary disk (e.g., GG tau, Piétu et al 2011;V4046 Sgr., Rodriguez et al 2010). In the second case (circumbinary disks), the orbital motion of the central binary is predicted to induce periodic perturbations, spiral density waves, and gas flows in the disk (Artymowicz & Lubow 1996;Larwood & Papaloizou 1997;Günther & Kley 2002;Günther et al 2004;Sotnikova & Grinin 2007;Hanawa et al 2010;Kaigorodov et al 2010;Alexander 2012;de Val-Borro et al 2011;Kocsis et al 2012). Characteristic features resulting from this interaction are inner cavities with the radius of about twice the semi-major axis of the binary (e.g., Artymowicz & Lubow 1994;Günther & Kley 2002).…”

Section: Introductionmentioning

confidence: 99%

Structures in circumbinary disks: Prospects for observability

Ruge

Wolf

Demidova

et al. 2015

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Context. During the past decade circumbinary disks have been discovered around various young binary stars. Hydrodynamical calculations indicate that the gravitational interaction between the central binary star and the surrounding disk results in global perturbations of the disk density profile. Aims. We study the observability of characteristic large-scale disk structures resulting from the binary-disk interaction in the case of close binary systems. Methods. We derived the structure of circumbinary disks from smoothed-particle hydrodynamic simulations. Subsequently, we performed radiative transfer simulations to obtain scattered light and thermal reemission maps. We investigated the influence of the binary mass ratio, the inclination of the binary orbit relative to the disk midplane, and the eccentricity of the binary orbit on observational quantities. Results. We find that ALMA will allow tracing asymmetries of the inner edge of the disk and potentially resolving spiral arms if the disk is seen face-on. For an edge-on orientation, ALMA will allow detecting perturbations in the disk density distribution through asymmetries in the radial brightness profile. Through the asymmetric structure of the disks, areas are formed with a temperature 2.6 times higher than at the same location in equivalent unperturbed disks. The time-dependent appearance of the density waves and spiral arms in the disk affects the total re-emission flux of the object by a few percent.

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“…

We have carried out 2D and 3D numerical simulations (Kaigorodov et al 2010 of accretion processes in binary T Tauri stars (TTSs) DQ Tau, UZ Tau E, V4046 Sgr, GW Ori, RoXs 42C using a finite-difference Roe-Osher-Einfeld TVD scheme. The morphology of the flow pattern for UZ Tau E is shown in Fig.

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confidence: 99%

Gas Dynamic Simulations of Inner Regions of Protoplanetary Disks in Young Binary Stars

et al. 2011

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We have carried out 2D and 3D numerical simulations (Kaigorodov et al. 2010 of accretion processes in binary T Tauri stars (TTSs) DQ Tau, UZ Tau E, V4046 Sgr, GW Ori, RoXs 42C using a finite-difference Roe-Osher-Einfeld TVD scheme. The morphology of the flow pattern for UZ Tau E is shown in Fig. 1 (left panel). The flow structure includes accretion disks surrounding the components, bow-shocks in front of both the components, a shock wave ("bridge") between the circumstellar accretion disks and a gap containing rarefied gas in the inner part of the protoplanetary disk.The performed simulations show that the radii of the gaps which formed due to the bow-shocks fit the observations better than the radii calculated using positions of the Linblad resonances according to Artymowicz & Lubow (1994). For systems with circular orbits, the calculated gap radius is ∼ 3A (A -semi-major axis of the system) and for those with elliptic orbits it is ∼ 3.2 -3.3A. Thus, the bow-shocks govern the size and shape of the gap in young binary systems.Analysis of the fluxes demonstrates that the re-distribution of the angular momentum in the envelope due to the bow-shocks leads to occurrence of two flows propagating from the inner edge of the protoplanetary disk to the components (see Fig. 1, right panel). Let us consider streams near the less massive star (secondary). The matter in the gap splits into two streams at the head-on collision point when passing through the bow-shock. The first portion of matter (stream A in Fig. 1, right panel) loses its angular momentum at the shock and starts to move toward the circumstellar accretion disk forming a spiral flow. The second portion of matter

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Structure of the circumbinary envelope around a young binary system

Cited by 31 publications

References 16 publications

Reverse rotation of the accretion disk in RW Aur A: Observations and a physical model

Reverse rotation of the accretion disk in RW Aur A: Observations and a physical model

Structures in circumbinary disks: Prospects for observability

Gas Dynamic Simulations of Inner Regions of Protoplanetary Disks in Young Binary Stars

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