Spirals in protoplanetary disks from photon travel time

Kama, M.; Pinilla, P.; Heays, A. N.

doi:10.1051/0004-6361/201628924

Cited by 16 publications

(27 citation statements)

References 37 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…• between the inner disk and 80 au (500 mas) if the responsible dust clump is located at 0.15 au (see also Kama et al 2016). Arguably, some of the shadow lanes show very minor tilts in Figure 2 but the precision and angular resolution of the observations challenge the identification of light travel time effects.…”

Section: Epoch 5 2016mentioning

confidence: 98%

Variable Dynamics in the Inner Disk of HD 135344B Revealed with Multi-epoch Scattered Light Imaging^∗

Stolker

Sitko

Lazareff

et al. 2017

ApJ

View full text Add to dashboard Cite

We present multi-epoch Very Large Telescope/Spectro-Polarimetric High-contrast Exoplanet REsearch observations of the protoplanetary disk around HD 135344B (SAO 206462). The J-band scattered light imagery reveal, with high spatial resolution (∼41 mas, 6.4 au), the disk surface beyond ∼20 au. Temporal variations are identified in the azimuthal brightness distributions of all epochs, presumably related to the asymmetrically shading dust distribution in the inner disk. These shadows manifest themselves as narrow lanes, cast by localized density enhancements, and broader features which possibly trace the larger scale dynamics of the inner disk. We acquired visible and near-infrared photometry which shows variations up to 10% in the JHK bands, possibly correlated with the presence of the shadows. Analysis of archival Very Large Telescope Interferometer/PIONIER H-band visibilities constrain the orientation of the inner disk to i = 18.• 2 +3.4−4.1 and PA = 57.• 3 ± 5.• 7, consistent with an alignment with the outer disk or a minor disk warp of several degrees. The latter scenario could explain the broad, quasi-stationary shadowing in N-NW direction in case the inclination of the outer disk is slightly larger. The correlation between the shadowing and the near-infrared excess is quantified with a grid of radiative transfer models. The variability of the scattered light contrast requires extended variations in the inner disk atmosphere (H/r 0.2). Possible mechanisms that may cause asymmetric variations in the optical depth (∆τ 1) through the atmosphere of the inner disk include turbulent fluctuations, planetesimal collisions, or a dusty disk wind, possibly enhanced by a minor disk warp. A fine temporal sampling is required to follow day-to-day changes of the shadow patterns which may be a face-on variant of the UX Orionis phenomenon.

show abstract

Section: Epoch 5 2016mentioning

confidence: 98%

Variable Dynamics in the Inner Disk of HD 135344B Revealed with Multi-epoch Scattered Light Imaging^∗

Stolker

Sitko

Lazareff

et al. 2017

ApJ

View full text Add to dashboard Cite

show abstract

“…While most discs would require uncomfortably high masses to explain the spiral morphology by self-gravity, this is nevertheless a possibility that cannot be excluded. There are also other alternative explanations for spiral arms, such as for example the finite light travel time from the star (Kama et al 2016) or the presence of shadows (Montesinos et al 2016).…”

Section: Introductionmentioning

confidence: 99%

Spiral arms in the protoplanetary disc HD100453 detected with ALMA: evidence for binary–disc interaction and a vertical temperature gradient

Rosotti

Benisty

Juhász

et al. 2019

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

Scattered light high-resolution imaging of the proto-planetary disc orbiting HD100453 shows two symmetric spiral arms, possibly launched by an external stellar companion. In this paper we present new, sensitive high-resolution (∼30 mas) Band 7 ALMA observations of this source. This is the first source where we find counterparts in the sub-mm continuum to both scattered light spirals. The CO J=3-2 emission line also shows two spiral arms; in this case they can be traced over a more extended radial range, indicating that the southern spiral arm connects to the companion position. This is clear evidence that the companion is responsible for launching the spirals. The pitch angle of the sub-millimeter continuum spirals (∼6 • ) is lower than the one in scattered light (∼16 • ). We show that hydrodynamical simulations of binary-disc interaction can account for the difference in pitch angle only if one takes into account that the midplane is colder than the upper layers of the disc, as expected for the case of externally irradiated discs.

show abstract

“…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%

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

Wagner

Dong

Sheehan

et al. 2018

ApJ

View full text Add to dashboard Cite

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.

show abstract

Spirals in protoplanetary disks from photon travel time

Cited by 16 publications

References 37 publications

Variable Dynamics in the Inner Disk of HD 135344B Revealed with Multi-epoch Scattered Light Imaging^∗

Variable Dynamics in the Inner Disk of HD 135344B Revealed with Multi-epoch Scattered Light Imaging^∗

Spiral arms in the protoplanetary disc HD100453 detected with ALMA: evidence for binary–disc interaction and a vertical temperature gradient

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

Contact Info

Product

Resources

About

Spirals in protoplanetary disks from photon travel time

Cited by 16 publications

References 37 publications

Variable Dynamics in the Inner Disk of HD 135344B Revealed with Multi-epoch Scattered Light Imaging∗

Variable Dynamics in the Inner Disk of HD 135344B Revealed with Multi-epoch Scattered Light Imaging∗

Spiral arms in the protoplanetary disc HD100453 detected with ALMA: evidence for binary–disc interaction and a vertical temperature gradient

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

Contact Info

Product

Resources

About

Variable Dynamics in the Inner Disk of HD 135344B Revealed with Multi-epoch Scattered Light Imaging^∗

Variable Dynamics in the Inner Disk of HD 135344B Revealed with Multi-epoch Scattered Light Imaging^∗