Spiral Waves Triggered by Shadows in Transition Disks

Montesinos, Matías; Pérez, Sebastián; Casassus, S.; Marino, Sebastián; Cuadra, Jorge; Christiaens, Valentin

doi:10.3847/2041-8205/823/1/l8

Cited by 101 publications

(115 citation statements)

References 32 publications

(59 reference statements)

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“…Spiral arms detected in scattered light have also been modeled as arising from rotating shadows cast by a warped inner disk (e.g., Montesinos et al 2016;Montesinos & Cuello 2018) and stellar flybys (e.g., Pfalzner 2003). These alternative explanations require specific conditions that are unlikely to be satisfied in the majority of cases.…”

Section: Discussionmentioning

confidence: 99%

Spiral Arms in Disks: Planets or Gravitational Instability?

Dong

Najita

Brittain

2018

ApJ

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Spiral arm structures seen in scattered-light observations of protoplanetary disks can potentially serve as signposts of planetary companions. They can also lend unique insights into disk masses, which are critical in setting the mass budget for planet formation but are difficult to determine directly. A surprisingly high fraction of disks that have been well studied in scattered light have spiral arms of some kind (8/29), as do a high fraction (6/11) of wellstudied Herbig intermediate-mass stars (i.e., Herbig stars >1.5 M e ). Here we explore the origin of spiral arms in Herbig systems by studying their occurrence rates, disk properties, and stellar accretion rates. We find that two-arm spirals are more common in disks surrounding Herbig intermediate-mass stars than are directly imaged giant planet companions to mature A and B stars. If two-arm spirals are produced by such giant planets, this discrepancy suggests that giant planets are much fainter than predicted by hot-start models. In addition, the high stellar accretion rates of Herbig stars, if sustained over a reasonable fraction of their lifetimes, suggest that disk masses are much larger than inferred from their submillimeter continuum emission. As a result, gravitational instability is a possible explanation for multiarm spirals. Future observations can lend insights into the issues raised here.

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Section: Discussionmentioning

confidence: 99%

Spiral Arms in Disks: Planets or Gravitational Instability?

Dong

Najita

Brittain

2018

ApJ

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“…SAO 206462 is an example of a young disc presenting spiral features that could be generated with either a planet or gravitational instability (Garufi et al 2013). Spiral waves may also be triggered by shadows in transition discs (Montesinos et al 2016), or even by an inflow coming from the residual external envelope of protoplanetary discs (Lesur et al 2015). We also note that mid-IR variability has been observed in many protoplanetary discs (Flaherty et al 2014).…”

Section: -Inhomogeneties In Protoplanetary Discmentioning

confidence: 74%

Effects of disc asymmetries on astrometric measurements

Kral

Kennedy

Souami

2016

A&A

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Astrometry covers a parameter space that cannot be reached by RV or transit methods to detect terrestrial planets on wide orbits. In addition, high accuracy astrometric measurements are necessary to measure the inclination of the planet's orbits. Here we investigate the principles of an artefact of the astrometric approach, namely the displacement of the photo-centre owing to inhomogeneities in a dust disc around the parent star. Indeed, theory and observations show that circumstellar discs can present strong asymmetries. We model the pseudo-astrometric signal caused by these inhomogeneities, asking whether a dust clump in a disc can mimic the astrometric signal of an Earth-like planet. We show that these inhomogeneities cannot be neglected when using astrometry to find terrestrial planets. We provide the parameter space for which these inhomogeneities can affect the astrometric signals but still not be detected by mid-IR observations. We find that a small cross section of dust corresponding to a cometary mass object is enough to mimic the astrometric signal of an Earth-like planet. Astrometric observations of protoplanetary discs to search for planets can also be affected by the presence of inhomogeneities. Some further tests are given to confirm whether an observation is a real astrometric signal from a planet or an impostor. Eventually, we also study the case where the cross-section of dust is high enough to provide a detectable IR-excess and to have a measurable photometric displacement by actual instruments such as Gaia, IRAC, or GRAVITY. We suggest a new method, which consists of using astrometry to quantify asymmetries (clumpiness) in inner debris discs that cannot be otherwise resolved.

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“…Thus, any dynamical model of the disk structure must include the effects of the companion's gravitational perturbations in order to accurately match the dynamics of the system. We suggest that the other proposed spiral-arm-producing mechanisms (e.g., Kama et al 2016;Montesinos et al 2016) are not responsible for the "grand design" spiral structure of HD 100453. Finally, we note that the inclinations of the various system components, with the exception of the inner disk, are consistent with a coplanar system.…”

Section: Discussionmentioning

confidence: 99%

“…Indeed, Montesinos et al (2016) provide an alternate mechanism for generating the spiral structure in this disk (further discussed in Benisty et al 2017) without invoking the gravitational perturbations from the companion, which may be the case if it is in fact on a much wider orbit. Thus, knowledge of the binary's true orbit may be used to discriminate between these hypotheses for the generation of the spiral arms, thereby providing constraints on the dynamics and evolution of this disk and, potentially, provide more general insights into disks with two-armed spiral structures.…”

Section: Introductionmentioning

confidence: 99%

“…Currently, there exist more alternate hypotheses for the generation of these features than sources to test their predictions. Most models include a massive perturbing companion (either a planet or a low-mass star, e.g., Dong et al 2015a andZhu et al 2015); though, notably, some do not require the presence of any companion (e.g., Kama et al 2016;Montesinos et al 2016;Benisty et al 2017).…”

Section: Introductionmentioning

confidence: 99%

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The Orbit of the Companion to HD 100453A: Binary-driven Spiral Arms in a Protoplanetary Disk

Wagner

Dong

Sheehan

et al. 2018

ApJ

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HD 100453AB is a 10±2 Myr old binary whose protoplanetary disk was recently revealed to host a global twoarmed spiral structure. Given the relatively small projected separation of the binary (1 05, or ∼108 au), gravitational perturbations by the binary seemed to be a likely driving force behind the formation of the spiral arms. However, the orbit of these stars remained poorly understood, which prevented a proper treatment of the dynamical influence of the companion on the disk. We observed HD100453AB between 2015 and 2017, utilizing extreme adaptive optics systems on the Very Large Telescope and the Magellan Clay Telescope. We combined the astrometry from these observations with published data to constrain the parameters of the binary's orbit to a = 1 06±0 09, e=0.17±0.07, and i = 32°.5 ± 6°.5. We utilized publicly available ALMA 12 CO data to constrain the inclination of the disk,~ i 28 disk , which is relatively coplanar with the orbit of the companion and consistent with previous estimates from scattered light images. Finally, we input these constraints into hydrodynamic and radiative transfer simulations to model the structural evolution of the disk. We find that the spiral structure and truncation of the circumprimary disk in HD 100453 are consistent with a companion-driven origin. Furthermore, we find that the primary star's rotation, its outer disk, and the companion exhibit roughly the same direction of angular momentum, and thus the system likely formed from the same parent body of material.

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Spiral Waves Triggered by Shadows in Transition Disks

Cited by 101 publications

References 32 publications

Spiral Arms in Disks: Planets or Gravitational Instability?

Spiral Arms in Disks: Planets or Gravitational Instability?

Effects of disc asymmetries on astrometric measurements

The Orbit of the Companion to HD 100453A: Binary-driven Spiral Arms in a Protoplanetary Disk

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