Publisher Note: Circumbinary, not transitional: On the spiral arms, cavity, shadows, fast radial flows, streamers and horseshoe in the HD142527 disc

Price, Daniel J.; Cuello, Nicolás; Pinte, C.; Mentiplay, Daniel; Casassus, S.; Christiaens, Valentin; Kennedy, Grant M.; Cuadra, Jorge; M., Sebastian Perez; Marino, Sebastián; Armitage, Philip J.; Zurlo, A.; Juhász, A.; Ragusa, Enrico; Laibe, Guillaume; Lodato, Giuseppe

doi:10.1093/mnras/sty2385

Cited by 7 publications

(5 citation statements)

References 81 publications

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“…Our numerical simulations, as well as previous theoretical models (Bate 2000;Günther & Kley 2002;Ochi et al 2005;Hanawa et al 2010;Shi et al 2012;Demidova & Shevchenko 2015;Young et al 2015;Price et al 2018), predict a two-arm spiral pattern in CBDs. The arms extend from the binaries through the L2 and L3 Lagrangian points in the Roche potential.…”

Section: Structures and Gas Motions In The Spiral Armssupporting

confidence: 76%

Circumbinary Disks of the Protostellar Binary Systems in the L1551 Region

Takakuwa,

Saigo,

Matsumoto

et al. 2020

Preprint

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We report ALMA Cycle 4 observations of the Class I binary protostellar system L1551 IRS 5 in the 0.9-mm continuum emission, C 18 O (J=3-2), OCS (J=28-27), and four other Band 7 lines. At ∼0. 07 (= 10 au) resolution in the 0.9 mm emission, two circumstellar disks (CSDs) associated with the binary protostars are separated from the circumbinary disk (CBD). The CBD is resolved into two spiral arms, one connecting to the CSD around the northern binary source, Source N, and the other to Source S. As compared to the CBD in the neighboring protobinary system L1551 NE, the CBD in L1551 IRS 5 is more compact (r ∼150 au) and the m=1 mode of the spirals found in L1551 NE is less obvious in L1551 IRS 5. Furthermore, the dust and molecular-line brightness temperatures of CSDs and CBD reach >260 K and >100 K, respectively, in L1551 IRS 5, much hotter than those in L1551 NE. The gas motions in the spiral arms are characterized by rotation and expansion. Furthermore, the transitions from the CBD to the CSD rotations at around the L2 and L3 Lagrangian points and gas motions around the L1 point are identified. Our numerical simulations reproduce the observed two spiral arms and expanding gas motion as a result of gravitational torques from the binary, transitions from the CBD to the CSD rotations, and the gas motion around the L1 point. The higher temperature in L1551 IRS 5 likely reflects the inferred FU-Ori event.

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Section: Structures and Gas Motions In The Spiral Armssupporting

confidence: 76%

Circumbinary Disks of the Protostellar Binary Systems in the L1551 Region

Takakuwa,

Saigo,

Matsumoto

et al. 2020

Preprint

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“…A theoretical understanding of CBD eccentricity profiles might aid the interpretation of observational data. Recently, the "binary interpretation" of transitional disks (Ireland & Kraus 2008) has attracted renewed interest as a result of the rich morphological and kinematic signatures observed in astrophysical disks (see., e.g., Price et al 2018, for the case of HD142527). Self-consistent eccentricity profiles will prove powerful tools as a diagnostic for hidden binaries and disk properties.…”

Section: Importance Of Eccentric Disksmentioning

confidence: 99%

Long-Lived Eccentric Modes in Circumbinary Disks

Muñoz,

Lithwick

2020

Preprint

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Hydrodynamical simulations show that circumbinary disks become eccentric, even when the binary is circular.Here we demonstrate that, in steady state, the disk's eccentricity behaves as a long-lived free mode of the disk. Consequently, both the disk's precession rate and eccentricity profile may be calculated via the simple linear theory for perturbed pressure-supported disks. By formulating and solving the linear theory we find that (i) surprisingly, the precession rate is roughly determined by the binary's quadrupole, even when the quadrupole is very weak relative to pressure; (ii) the eccentricity profile is largest near the inner edge of the disk, and falls exponentially outwards; and (iii) the results from linear theory indeed agree with what is found in simulations. Understanding the development of eccentric modes in circumbinary disks is a crucial first step for understanding the long term (secular) exchange of eccentricity, angular momentum and mass between the binary and the gas. Potential applications include the search for a characteristic kinematic signature in disks around candidate binaries and precession-induced modulation of accretion over long timescales.

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“…Regály et al 2012;Lyra & Mac Low 2012;Miranda et al 2017). Furthermore, alternate ideas such as the presence of a close-in companion star adding eccentricity to the disc (Ataiee et al 2013;Ragusa et al 2017;Price et al 2018) are also possible. These scenarios that do not rely on planets may still prove to be better explanations for some, if not all of these asymmetries.…”

Section: Introductionmentioning

confidence: 99%

Observational diagnostics of elongated planet-induced vortices with realistic planet formation time-scales

Hammer

Pinilla

Kratter

et al. 2018

Monthly Notices of the Royal Astronomical Society

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Gap-opening planets can generate dust-trapping vortices that may explain some of the latest discoveries of high-contrast crescent-shaped dust asymmetries in transition discs. While planet-induced vortices were previously thought to have concentrated shapes, recent computational work has shown that these features naturally become much more elongated in the gas when simulations account for the relatively long timescale over which planets accrete their mass. In this work, we conduct two-fluid hydrodynamical simulations of vortices induced by slowly-growing Jupiter-mass planets in discs with very low viscosity (α = 3×10 −5 ). We simulate the dust dynamics for four particle sizes spanning 0.3 mm to 1 cm in order to produce synthetic ALMA images. In our simulations, we find that an elongated vortex still traps dust, but not directly at its center. With a flatter pressure bump and disruptions from the planet's overlapping spiral density waves, the dust instead circulates around the vortex. This motion (1) typically carries the peak off-center, (2) spreads the dust out over a wider azimuthal extent 180 • , (3) skews the azimuthal profile towards the front of the vortex, and (4) can also create double peaks in newly-formed vortices. In particular, we expect that the most defining observational signature, a peak offset of more than 30 • , should be detectable > 30% of the time in observations with a beam diameter of at most the planet's separation from its star.

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Publisher Note: Circumbinary, not transitional: On the spiral arms, cavity, shadows, fast radial flows, streamers and horseshoe in the HD142527 disc

Cited by 7 publications

References 81 publications

Circumbinary Disks of the Protostellar Binary Systems in the L1551 Region

Circumbinary Disks of the Protostellar Binary Systems in the L1551 Region

Long-Lived Eccentric Modes in Circumbinary Disks

Observational diagnostics of elongated planet-induced vortices with realistic planet formation time-scales

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