A triple-star system with a misaligned and warped circumstellar disk shaped by disk tearing

Kraus, Stefan; Kreplin, Alexander; Young, Alison K.; Bate, Matthew R.; Monnier, John D.; Harries, Tim J.; Avenhaus, H.; Kluska, J.; Laws, Anna; Rich, Evan A.; Willson, Matthew; Aarnio, Alicia; Adams, Fred C.; Andrews, Sean M.; Anugu, Narsireddy; Bae, Jaehan; Brummelaar, T. ten; Calvet, Nuria; Curé, M.; Davies, Claire L.; Ennis, Jacob; Espaillat, Catherine; Gardner, Tyler; Hartmann, L.; Hinkley, Sasha; Labdon, Aaron; Lanthermann, Cyprien; Bouquin, J.-B. Le; Schaefer, Gail H.; Setterholm, Benjamin R.; Wilner, David J.; Zhu, Zhaohuan

doi:10.1126/science.aba4633

Cited by 94 publications

(73 citation statements)

References 76 publications

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“…Indeed some of the observed warped protoplanetary discs are strongly misaligned, suggesting that disc breaking may have occurred (see, e.g. Marino et al 2015;Kraus et al 2020).…”

Section: Discussionmentioning

confidence: 99%

Parametric instability in a free-evolving warped protoplanetary disc

Deng

Ogilvie

Mayer

2020

Monthly Notices of the Royal Astronomical Society

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Warped accretion discs of low viscosity are prone to hydrodynamic instability due to parametric resonance of inertial waves as confirmed by local simulations. Global simulations of warped discs, using either smoothed particle hydrodynamics (SPH) or grid-based codes, are ubiquitous but no such instability has been seen. Here we utilize a hybrid Godunov-type Lagrangian method to study parametric instability in global simulations of warped Keplerian discs at unprecedentedly high resolution (up to 120 million particles). In the global simulations, the propagation of the warp is well described by the linear bending-wave equations before the instability sets in. The ensuing turbulence, captured for the first time in a global simulation, damps relative orbital inclinations and leads to a decrease in the angular momentum deficit. As a result, the warp undergoes significant damping within one bending-wave crossing time. Observed protoplanetary disc warps are likely maintained by companions or aftermath of disc breaking.

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“…Indeed some of the observed warped protoplanetary discs are strongly misaligned, suggesting that disc breaking may have occurred (see, e.g. Marino et al 2015;Kraus et al 2020).…”

Section: Discussionmentioning

confidence: 99%

Parametric instability in a free-evolving warped protoplanetary disc

Deng

Ogilvie

Mayer

2020

Monthly Notices of the Royal Astronomical Society

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“…The dust emission comes mostly from two coplanar outer rings with the radii of 180 and 350 au and from the tilted inner ring of 43 au radius. Interferometric observations in the mm range and high-contrast imaging in the IR revealed the 3D structure of these rings in unprecedented detail [90]. All rings rotate in the same sense, but the inner ring is inclined to the outer orbit of the triple by 39 • .…”

Section: Young Hierarchiesmentioning

confidence: 97%

Architecture of Hierarchical Stellar Systems and Their Formation

Tokovinin

2021

Universe

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Accumulation of new data on stellar hierarchical systems and the progress in numerical simulations of their formation open the door to genetic classification of these systems, where properties of a certain group (family) of objects are tentatively related to their formation mechanisms and early evolution. A short review of the structure and statistical trends of known stellar hierarchies is given. Like binaries, they can be formed by the disk and core fragmentation events happening sequentially or simultaneously and followed by the evolution of masses and orbits driven by continuing accretion of gas and dynamical interactions between stars. Several basic formation scenarios are proposed and associated qualitatively with the architecture of real systems, although quantitative predictions for these scenarios are still pending. The general trend of increasing orbit alignment with decreasing system size points to the critical role of the accretion-driven orbit migration, which also explains the typically comparable masses of stars belonging to the same system. The architecture of some hierarchies bears imprints of chaotic dynamical interactions. Characteristic features of each family are illustrated by several real systems.

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“…have not yet turned up any examples of a misaligned star however, there are hints, albeit limited, from (32) who found evidence that 1/3 of their sample had non-aligned configurations. There are some cases in which the inner and outer disk are misaligned, and obviously the star must be misaligned with one of them (33). For now, the architecture of the K2-290 system shows that we cannot safely assume that stars and their protoplanetary disks are always well aligned.…”

Section: Discussionmentioning

confidence: 98%

A backward-spinning star with two coplanar planets

Hjorth

Albrecht

Hirano

et al. 2021

Proc. Natl. Acad. Sci. U.S.A.

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It is widely assumed that a star and its protoplanetary disk are initially aligned, with the stellar equator parallel to the disk plane. When observations reveal a misalignment between stellar rotation and the orbital motion of a planet, the usual interpretation is that the initial alignment was upset by gravitational perturbations that took place after planet formation. Most of the previously known misalignments involve isolated hot Jupiters, for which planet–planet scattering or secular effects from a wider-orbiting planet are the leading explanations. In theory, star/disk misalignments can result from turbulence during star formation or the gravitational torque of a wide-orbiting companion star, but no definite examples of this scenario are known. An ideal example would combine a coplanar system of multiple planets—ruling out planet–planet scattering or other disruptive postformation events—with a backward-rotating star, a condition that is easier to obtain from a primordial misalignment than from postformation perturbations. There are two previously known examples of a misaligned star in a coplanar multiplanet system, but in neither case has a suitable companion star been identified, nor is the stellar rotation known to be retrograde. Here, we show that the star K2-290 A is tilted by 124○±6○ compared with the orbits of both of its known planets and has a wide-orbiting stellar companion that is capable of having tilted the protoplanetary disk. The system provides the clearest demonstration that stars and protoplanetary disks can become grossly misaligned due to the gravitational torque from a neighboring star.

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A triple-star system with a misaligned and warped circumstellar disk shaped by disk tearing

Cited by 94 publications

References 76 publications

Parametric instability in a free-evolving warped protoplanetary disc

Parametric instability in a free-evolving warped protoplanetary disc

Architecture of Hierarchical Stellar Systems and Their Formation

A backward-spinning star with two coplanar planets

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