GW Ori: Interactions between a Triple-star System and Its Circumtriple Disk in Action

Bi, Jiaqing; Marel, Nienke van der; Dong, Ruobing; Muto, Takayuki; Martin, Rebecca G.; Smallwood, Jeremy L.; Hashimoto, Jun; Liu, Hauyu Baobab; Nomura, Hideko; Hasegawa, Yasuhiro; Takami, M.; Konishi, Mihoko; Momose, Munetake; Kanagawa, Kazuhiro D.; Kataoka, Akimasa; Ono, Tomohiro; Sitko, Michael L.; Takahashi, Sanemichi Z.; Tomida, Kengo; Tsukagoshi, Takashi

doi:10.3847/2041-8213/ab8eb4

Cited by 56 publications

(58 citation statements)

References 48 publications

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“…Recent observations of the triple star system GW Orionis have shown a peculiar geometry, consisting of a circumtriple broken misaligned disc with three dust rings (Bi et al 2020;Kraus et al 2020). GW Orionis is a young hierarchical triple stellar system (1 ± 0.1Myr, Calvet et al (2004)) in the Orion Molecular Cloud at a distance of 388 ± 5pc (Kounkel et al 2017).…”

Section: The Case Of Gw Orionismentioning

confidence: 99%

Dynamical dust traps in misaligned circumbinary discs: analytical theory and numerical simulations

Longarini

Lodato

Toci

et al. 2021

Monthly Notices of the Royal Astronomical Society

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Recent observations have shown that circumbinary discs can be misaligned with respect to the binary orbital plane.The lack of spherical symmetry, together with the non-planar geometry of these systems, causes differential precession which might induce the propagation of warps. While gas dynamics in such environments is well understood, little is known about dusty discs. In this work, we analytically study the problem of dust traps formation in misaligned circumbinary discs. We find that pile-ups may be induced not by pressure maxima, as the usual dust traps, but by a difference in precession rates between the gas and dust. Indeed, this difference makes the radial drift inefficient in two locations, leading to the formation of two dust rings whose position depends on the system parameters. This phenomenon is likely to occur to marginally coupled dust particles (St ≳ 1) as both the effect of gravitational and drag force are considerable. We then perform a suite of three-dimensional SPH numerical simulations to compare the results with our theoretical predictions. We explore the parameter space, varying stellar mass ratio, disc thickness, radial extension, and we find a general agreement with the analytical expectations. Such dust pile-up prevents radial drift, fosters dust growth and may thus promote the planet formation in circumbinary discs.

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Section: The Case Of Gw Orionismentioning

confidence: 99%

Dynamical dust traps in misaligned circumbinary discs: analytical theory and numerical simulations

Longarini

Lodato

Toci

et al. 2021

Monthly Notices of the Royal Astronomical Society

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“…GW Ori is a triple star system that includes a misaligned circumtriple disc. With ALMA observations, three dust rings which have different mutual inclinations (> 10 • ) to the stars have been identified (Bi et al 2020;Kraus et al 2020). An initially misaligned disc that is not at a stationary inclination around an eccentric orbit binary undergoes tilt oscillations, even if it is evolving towards coplanarity (Smallwood et al 2019), and may evolve towards a more misaligned (polar) configuration with respect to the binary, such as in HD98800 (Kennedy et al 2019).…”

Section: Discussionmentioning

confidence: 99%

Orbital dynamics of two circumbinary planets around misaligned eccentric binaries

Chen,

Lubow,

Martin

2021

Preprint

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We investigate the orbital dynamics of circumbinary planetary systems with two planets around a circular or eccentric orbit binary. The orbits of the two planet are initially circular and coplanar to each other, but misaligned with respect to the binary orbital plane. The binaryplanet and planet-planet interactions result in complex planet tilt oscillations. We use analytic models and numerical simulations to explore the effects of various values of the planet semimajor axes, binary eccentricity, and initial inclination. Around a circular orbit binary, secular tilt oscillations are driven by planet-planet interactions and are periodic. In that case, planets undergo mutual libration if close together and circulation if far apart with an abrupt transition at a critical separation. Around an eccentric orbit binary, secular tilt oscillations are driven by both planet-planet interactions and binary-planet interactions. These oscillations generally display more than one frequency and are generally not periodic. The transition from mutual planet libration to circulation is not sharp and there is a range of separations for which the planets are on orbits that are sometimes mutually librating and sometimes circulating. In addition, at certain separations, there are resonances for which tilt oscillations are complicated but periodic. For planets that are highly misaligned with respect to an eccentric orbit binary, there are stationary (non-oscillating) tilt configurations that are generalisations of polar configurations for the single planet case. Tilt oscillations of highly inclined planets occur for initial tilts that depart from the stationary configuration.

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“…06 5 . This offset could be explained if the dust ring is eccentric, a feature naturally produced through binary-disk interaction (e.g., GW Ori, Bi et al 2020;Kraus et al 2020). In the 8 mm image, emission from (or close to) the two stars is marginally resolved and well separated from the dust ring.…”

Section: Dust Diskmentioning

confidence: 99%

The Architecture of the V892 Tau System: the Binary and its Circumbinary Disk

Long,

Andrews,

Vega

et al. 2021

Preprint

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We present high resolution millimeter continuum and CO line observations for the circumbinary disk around V892 Tau to constrain the stellar and disk properties. The total mass of the two near-equalmass A stars is estimated to be 6.0 ± 0.2 M based on our models of the Keplerian-dominated gas disk rotation. The detection of strong ionized gas emission associated with the two stars at 8 mm, when combined with previous astrometric measurements in the near-infrared, provides an updated view of the binary orbit with a = 7.1 ± 0.1 au, e = 0.27 ± 0.1, and P = 7.7 ± 0.2 yr, which is about half of a previously reported orbital period. The binary orbital plane is proposed to be near coplanar to the circumbinary disk plane (with a mutual inclination of only ∆ = 8 ± 4.2 • ; another solution with ∆ = 113 • is less likely given the short re-alignment timescale). An asymmetric dust disk ring peaking at a radius of 0. 2 is detected at 1.3 mm and its fainter counterparts are also detected at the longer 8 and 9.8 mm. The CO gas disk, though dominated by Keplerian rotation, presents a mild inner and outer disk misalignment. The radial extension of the disk, its asymmetric dust ring, and the presence of a disk warp could all be explained by the interaction between the eccentric binary and the circumbinary disk, which we assume were formed with non-zero mutual inclination. Some tentatively detected gas spirals in the outer disk are likely produced by interactions with the low mass tertiary component located 4 to the northeast. Our analyses demonstrate the promising usage of V892 Tau as an excellent benchmark system to study the details of binary-disk interactions.

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GW Ori: Interactions between a Triple-star System and Its Circumtriple Disk in Action

Cited by 56 publications

References 48 publications

Dynamical dust traps in misaligned circumbinary discs: analytical theory and numerical simulations

Dynamical dust traps in misaligned circumbinary discs: analytical theory and numerical simulations

Orbital dynamics of two circumbinary planets around misaligned eccentric binaries

The Architecture of the V892 Tau System: the Binary and its Circumbinary Disk

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