Structures in circumbinary disks: Prospects for observability

Ruge, Jan Philipp; Wolf, S.; Demidova, T. V.; Гринин, В. П.

doi:10.1051/0004-6361/201321770

Cited by 13 publications

(17 citation statements)

References 63 publications

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“…From this we conclude that the wavelength of the density wave has a greater influence on the detectability than the wave magnitude. Finally, we want to compare our results to a similar study performed by Ruge et al (2015). One of the major differences of our work compared to the results of Ruge et al (2015) is the lack of density waves.…”

Section: Almamentioning

confidence: 84%

“…Finally, we want to compare our results to a similar study performed by Ruge et al (2015). One of the major differences of our work compared to the results of Ruge et al (2015) is the lack of density waves. There are three major reasons for this.…”

Section: Almamentioning

confidence: 84%

“…The first reason is the difference in the simulations. Ruge et al (2015) conducted a SPH simulation of the inner disk regions. The hydrodynamic simulation performed in this study achieves a better resolution, which allows us to track smaller structures.…”

Section: Almamentioning

confidence: 99%

“…This leads to a change in basic physical properties of the circumbinary disk, which should in turn result in unique structures such as a cavity in the disk centre, accretion arms, density waves, and spiral arms (Günther & Kley 2002;Günther et al 2004). Previously it was shown that some of these structures, such as the cavity and parts of the accretion arms, are observable with the current generation of instruments (Ruge et al 2015). There are also examples of more complex systems, such as GG Tau, which is a triple star system (Piétu et al 2011;Di Folco et al 2014).…”

Section: Introductionmentioning

confidence: 99%

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Observability of characteristic binary-induced structures in circumbinary disks

Avramenko

Wolf

Illenseer

2017

A&A

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Context. A substantial fraction of protoplanetary disks form around stellar binaries. The binary system generates a time-dependent non-axisymmetric gravitational potential, inducing strong tidal forces on the circumbinary disk. This leads to a change in basic physical properties of the circumbinary disk, which should in turn result in unique structures that are potentially observable with the current generation of instruments. Aims. The goal of this study is to identify these characteristic structures, constrain the physical conditions that cause them, and evaluate the feasibility of observing them in circumbinary disks. Methods. To achieve this, first we perform 2D hydrodynamic simulations. The resulting density distributions are post-processed with a 3D radiative transfer code to generate re-emission and scattered light maps. Based on these distributions, we study the influence of various parameters, such as the mass of the stellar components, mass of the disk, and binary separation on observable features in circumbinary disks. Results. We find that the Atacama Large (sub-)Millimetre Array (ALMA) as well as the European Extremely Large Telescope (E-ELT) are capable of tracing asymmetries in the inner region of circumbinary disks, which are affected most by the binary-disk interaction. Observations at submillimetre/millimetre wavelengths allow the detection of the density waves at the inner rim of the disk and inner cavity. With the E-ELT one can partially resolve the innermost parts of the disk in the infrared wavelength range, including the disk's rim, accretion arms, and potentially the expected circumstellar disks around each of the binary components.

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Section: Almamentioning

confidence: 84%

Section: Almamentioning

confidence: 84%

Section: Almamentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Observability of characteristic binary-induced structures in circumbinary disks

Avramenko

Wolf

Illenseer

2017

A&A

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“…Occasionally, simple schematic models that were not based on hydrodynamic calculations were used to calculate the asymmetry in disk images (Flaherty & Muzerolle 2010). Our works (Demidova & Grinin 2014;Ruge et al 2015) differ in that we obtained the theoretical images of protoplanetary disks in the infrared and submillimeter spectral ranges based on the hydrodynamic models computed by the SPH method.…”

Section: Introductionmentioning

confidence: 99%

SPH simulations of structures in protoplanetary disks

Demidova

Гринин

2017

Astron. Lett.

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The hydrodynamic models of the protoplanetary disk, which perturbed by the embeded low-mass companion, were calculated by our modification of GADGET-2 code. The cases of circular and eccentric orbits which can be coplanar or slightly inclined to the disk midplane were considered. The column density of test particles on the line of sight between the central star and observer was computed during the simulations. Then the column density of the circumstellar dust was calculated under the assumption that the dust and gas are well mixed with a mass ratio 1 : 100. To research the influence of the disk orientation relative to the observer on the circumstellar extinction the calculations were made for four angles of inclination of the line of sight to the disk midplane and eight directions along the azimuth. The column density in the circumstellar and circumbinary disk were computed separately. The calculations have shown the periodic variations of column density can arise both in the circumstellar and circumbinary disks. The amplitude and shape of the variation strongly depend on the parameters of the simulated system (eccentricity and inclination of the orbit, the mass ratio of the companion and star) and its orientation in space. The results of our simulations can be used to explain the cyclic variation of the brightness of young UX Ori type stars.

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Selected aspects of the analysis of molecular line observations of edge-on circumbinary disks

Avramenko¹,

Wolf²,

Illenseer³

et al. 2020

A&A

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Context. Inner cavities, accretion arms, and density waves are characteristic structures in the density distribution of circumbinary disks. They are the result of the tidal interaction of the non-axisymmetric gravitational forces of the central binary with the surrounding disk and are most prominent in the inner region, where the asymmetry is most pronounced. Aims. The goal of this study is to test the feasibility of reconstructing the gas density distribution and quantifying properties of structures in the inner regions of edge-on circumbinary disks using multiple molecular line observations. Methods. The density distribution in circumbinary disks is calculated with 2D hydrodynamic simulations. Subsequently, molecular line emission maps are generated with 3D radiative transfer simulations. Based on these, we investigate the observability of characteristic circumbinary structures located in the innermost region for spatially resolved and unresolved disks. Results. We find that it is possible to reconstruct the inner cavity, accretion arms, and density waves from spatially resolved multi-wavelength molecular line observations of circumbinary disks seen edge-on. For the spatially unresolved observations only, an estimate can be derived for the density gradient in the transition area between the cavity and the disk’s inner rim.

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Structures in circumbinary disks: Prospects for observability

Cited by 13 publications

References 63 publications

Observability of characteristic binary-induced structures in circumbinary disks

Observability of characteristic binary-induced structures in circumbinary disks

SPH simulations of structures in protoplanetary disks

Selected aspects of the analysis of molecular line observations of edge-on circumbinary disks

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