On the cavity size in circumbinary discs

Hirsh, Kieran; Price, Daniel J.; Gonzalez, Jean-François; Gabellini, Maria Giulia Ubeira; Ragusa, Enrico

doi:10.1093/mnras/staa2536

Cited by 42 publications

(40 citation statements)

References 65 publications

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“…size and eccentricity, has been documented in numerical works (Thun et al 2017;Hirsh et al 2020;Ragusa et al 2020). Results suggested that the gas cavity profile progressively steepens to match the theoretical prediction (Hirsh et al 2020). A large disc thickness (we recall in this case 𝐻/𝑅 = 0.2) and viscosity 𝛼 ss appear to prevent the disc eccentricity to reach large values in the gas (Ragusa et al 2020), as it would be instead expected for lower disc aspect ratios (Thun et al 2017;Miranda et al 2017).…”

Section: Kinematics and Evolution Of The System Propertiessupporting

confidence: 58%

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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: Kinematics and Evolution Of The System Propertiessupporting

confidence: 58%

“…Long term evolution of the cavity properties, i.e. size and eccentricity, has been documented in numerical works (Thun et al 2017;Hirsh et al 2020;Ragusa et al 2020). Results suggested that the gas cavity profile progressively steepens to match the theoretical prediction (Hirsh et al 2020).…”

Section: Kinematics and Evolution Of The System Propertiesmentioning

confidence: 88%

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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“…Harris et al 2012) or multiple Jovian planets (Dodson-Robinson & Salyk 2011; Close 2020). A binary companion can clear a cavity of 2-5 times the binary separation (Artymowicz & Lubow 1994;Hirsh et al 2020), so for transition disk cavities of ∼25-100 au we are interested in binary companions at ∼10-50 au separation. This is further discussed in Section 6.5.…”

Section: Observed Disk Morphologies Exoplanet Demographicsmentioning

confidence: 99%

A stellar mass dependence of structured disks: a possible link with exoplanet demographics

van der Marel,

Mulders

2021

Preprint

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Gaps in protoplanetary disks have long been hailed as signposts of planet formation. However, a direct link between exoplanets and disks remains hard to identify. We present a large sample study of ALMA disk surveys of nearby starforming regions to disentangle this connection. All disks are classified as either structured (transition, ring, extended) or non-structured (compact) disks. Although low-resolution observations may not identify large scale substructure, we assume that an extended disk must contain substructure from a dust evolution argument. A comparison across ages reveals that structured disks retain high dust masses up to at least 10 Myr, whereas the dust mass of compact, non-structured disks decreases over time. This can be understood if the dust mass evolves primarily by radial drift, unless drift is prevented by pressure bumps. We identify a stellar mass dependence of the fraction of structured disks. We propose a scenario linking this dependence with that of giant exoplanet occurrence rates. We show that there are enough exoplanets to account for the observed disk structures if transitional disks are created by exoplanets more massive than Jupiter, and ring disks by exoplanets more massive than Neptune, under the assumption that most of those planets eventually migrate inwards. On the other hand, the known anti-correlation between transiting super-Earths and stellar mass implies those planets must form in the disks without observed structure, consistent with formation through pebble accretion in drift-dominated disks. These findings support an evolutionary scenario where the early formation of giant planets determines the disk's dust evolution and its observational appearance.

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“…We assume that the disk with i d = 54.6 • and Ω d = 53.0 • has its NW side closer to the observer. Following this definition, due to the 180 • ambiguity of Ω b , we obtain two possible solutions (see Figure 10 Theoretical models of tidal truncation predict that the inner edges (r in ) of circumbinary disks would be located at 2-3a for binary orbits with moderate eccentricity and when coplanar with their surrounding disks (Artymowicz & Lubow 1994;Hirsh et al 2020). In the case of misalignment, r in /a would however have a complicated dependence on the mutual inclination, orbital eccentricity, and binary mass ratio.…”

Section: V892 Taumentioning

confidence: 99%

“…Depending on the stellar configuration, multiple disks could be present in a binary system, including a circumbinary disk orbiting around the binary and disks surrounding individual stellar components. Dynamical interactions between stars and disks tend to truncate the disks (e.g., creating an inner cavity in a circumbinary disk), reduce their masses, and shorten their lifetimes (e.g., Artymowicz & Lubow 1994;Breslau et al 2014;Hirsh et al 2020). For example, disks in close binaries (separation < 30 − 40 au) have fainter millimeter emission (Jensen et al 1996;Harris et al 2012;Akeson et al 2019), with a lower frequency presenting accretion signatures and/or near-infrared excess emission (Bouwman et al 2006;Cieza et al 2009;Kraus et al 2012), compared to disks around single stars.…”

Section: Introductionmentioning

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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On the cavity size in circumbinary discs

Cited by 42 publications

References 65 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

A stellar mass dependence of structured disks: a possible link with exoplanet demographics

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

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