Binary-induced spiral arms inside the disc cavity of AB Aurigae

Poblete, Pedro P.; Calcino, Josh; Cuello, Nicolás; Macías, Enrique; Ribas, Álvaro; Price, Daniel J.; Cuadra, Jorge; Pinte, C.

doi:10.1093/mnras/staa1655

Cited by 34 publications

(27 citation statements)

References 75 publications

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“…We can safely exclude the 𝜃 = 60 • case, because both the reduced cavity size and the lack of azimuthal over-density make this case significantly different from the observations. Non-coplanarity between the binary and the circumbinary disc has been previously invoked to explain the morphology in a number of systems (Price et al 2018b;Calcino et al 2020;Poblete et al 2020;Ballabio et al 2021). This highlights that misaligned geometries are not particularly exotic and is in agreement with the results by Czekala et al (2019), who found that distribution of binary-disc inclination is relatively flat for long period binaries.…”

Section: Discussionsupporting

confidence: 85%

Circumbinary and circumstellar discs around the eccentric binary IRAS 04158+2805 — a testbed for binary–disc interaction

Ragusa

Fasano

Toci

et al. 2021

Monthly Notices of the Royal Astronomical Society

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IRAS 04158+2805 has long been thought to be a very low mass T-Tauri star (VLMS) surrounded by a nearly edge-on, extremely large disc. Recent observations revealed that this source hosts a binary surrounded by an extended circumbinary disc with a central dust cavity. In this paper, we combine ALMA multi-wavelength observations of continuum and 12CO line emission, with Hα imaging and Keck astrometric measures of the binary to develop a coherent dynamical model of this system. The system features an azimuthal asymmetry detected at the western edge of the cavity in Band 7 observations and a wiggling outflow. Dust emission in ALMA Band 4 from the proximity of the individual stars suggests the presence of marginally resolved circumstellar discs. We estimate the binary orbital parameters from the measured arc of the orbit from Keck and ALMA astrometry. We further constrain these estimates using considerations from binary-disc interaction theory. We finally perform three SPH gas + dust simulations based on the theoretical constraints; we post-process the hydrodynamic output using radiative transfer Monte Carlo methods and directly compare the models with observations. Our results suggest that a highly eccentric e ∼ 0.5–0.7 equal mass binary, with a semi-major axis of ∼55 au, and small/moderate orbital plane versus circumbinary disc inclination θ ≲ 30○ provides a good match with observations. A dust mass of ∼1.5 × 10−4 M⊙ best reproduces the flux in Band 7 continuum observations. Synthetic CO line emission maps qualitatively capture both the emission from the central region and the non-Keplerian nature of the gas motion in the binary proximity.

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Section: Discussionsupporting

confidence: 85%

Circumbinary and circumstellar discs around the eccentric binary IRAS 04158+2805 — a testbed for binary–disc interaction

Ragusa

Fasano

Toci

et al. 2021

Monthly Notices of the Royal Astronomical Society

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“…These illumination features are thought to be caused by a misaligned inner disc that obstructs the stellar light (Marino et al 2015;Min et al 2017). The detailed modelling of individual sources, such as HD 142527 (Price et al 2018b) and AB Aur (Poblete et al 2020), shows how a circumprimary disc can form from the infalling material in the presence of an eccentric and inclined companion inside the disc cavity.…”

Section: Discussionmentioning

confidence: 99%

Spirals, shadows, and precession in HD 100453 – I. The orbit of the binary

Gonzalez

Plas

Pinte

et al. 2020

Monthly Notices of the Royal Astronomical Society

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In recent years, several protoplanetary discs have been observed to exhibit spirals, both in scattered light and (sub)millimetre continuum data. The HD 100453 binary star system hosts such a disc around its primary. Previous work has argued that the spirals were caused by the gravitational interaction of the secondary, which was assumed to be on a circular orbit, coplanar with the disc (meaning here the large outer disc, as opposed to the very small inner disc). However, recent observations of the CO gas emission were found incompatible with this assumption. In this paper, we run SPH simulations of the gas and dust disc for seven orbital configurations taken from astrometric fits and compute synthetic observations from their results. Comparing to high-resolution ALMA 12CO data, we find that the best agreement is obtained for an orbit with eccentricity e = 0.32 and semi-major axis a = 207 au, inclined by 61○ relative to the disc plane. The large misalignment between the disc and orbit planes is compatible with the tidal evolution of a circumprimary disc in an eccentric, unequal-mass binary star.

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“…Pinte et al 2018Pinte et al , 2019 and stellar companions (e.g. Calcino et al 2019;Poblete et al 2020) in the disc. Determining the origin of the twist in MWC 758 will help refine our model, as whether it originates due to an inclined inner disc, or radial flows, can imply different consequences for our companion (e.g.…”

Section: Co Emissionmentioning

confidence: 99%

“…We acknowledge use of the OzStar supercomputing facility, funded by Swinburne University and the Australian Government. we used SPLASH and PLONK for visualisation of our simulations (Price 2007;Mentiplay 2019).…”

Section: Acknowledgementsmentioning

confidence: 99%

Are the spiral arms in the MWC 758 protoplanetary disc driven by a companion inside the cavity?

Calcino

Christiaens

Price

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Spiral arms in protoplanetary discs are thought to be linked to the presence of companions. We test the hypothesis that the double spiral arm morphology observed in the transition disc MWC 758 can be generated by an ≈10 MJup companion on an eccentric orbit internal to the spiral arms. Previous studies on MWC 758 have assumed an external companion. We compare simulated observations from three dimensional hydrodynamics simulations of disc-companion interaction to scattered light, infrared and CO molecular line observations, taking into account observational biases. The inner companion hypothesis is found to explain the double spiral arms, as well as several additional features seen in MWC 758 — the arc in the northwest, substructures inside the spiral arms, the cavity in CO isotopologues, and the twist in the kinematics. Testable predictions include detection of fainter spiral structure, detection of a point source south-southeast of the primary, and proper motion of the spiral arms.

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Binary-induced spiral arms inside the disc cavity of AB Aurigae

Cited by 34 publications

References 75 publications

Circumbinary and circumstellar discs around the eccentric binary IRAS 04158+2805 — a testbed for binary–disc interaction

Circumbinary and circumstellar discs around the eccentric binary IRAS 04158+2805 — a testbed for binary–disc interaction

Spirals, shadows, and precession in HD 100453 – I. The orbit of the binary

Are the spiral arms in the MWC 758 protoplanetary disc driven by a companion inside the cavity?

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