The Missing Cavities in the Seeds Polarized Scattered Light Images of Transitional Protoplanetary Disks: A Generic Disk Model

Dong, Ruobing; Rafikov, Roman R.; Zhu, Zhaohuan; Hartmann, L.; Whitney, B. A.; Brandt, Timothy D.; Muto, Takayuki; Hashimoto, Jun; Grady, C. A.; Follette, Katherine B.; Kuzuhara, Masayuki; Tanii, Ryoko; Itoh, Yoichi; Thalmann, Christian; Wisniewski, John P.; Mayama, Satoshi; Janson, Markus; Abe, Lyu; Brandner, W.; Carson, J.; Egner, Sebastian; Feldt, M.; Goto, Miwa; Guyon, Olivier; Hayano, Yutaka; Hayashi, Masahiko; Hayashi, Saeko S.; Henning, Th.; Hodapp, Klaus W.; Honda, Mitsuhiko; Inutsuka, Shu Ichi; Ishii, Miki; Iye, Masanori; Kandori, Ryo; Knapp, G. R.; Kudo, Tomoyuki; Kusakabe, Nobuhiko; Matsuo, Taro; McElwain, Michael W.; Miyama, Shoken M.; Morino, Jun-Ichi; Moro‐Martín, Amaya; Nishimura, Tetsuo; Pyo, Tae‐Soo; Shimada, Hiroshi; Suzuki, Ryuji; Takami, M.; Takato, Naruhisa; Terada, Hiroshi; Tomono, Daigo; Turner, Edwin L.; Watanabe, Makoto; Yamada, Tōru; Takami, Hideki; Usuda, Tomonori; Tamura, Motohide

doi:10.1088/0004-637x/750/2/161

Cited by 117 publications

(89 citation statements)

References 57 publications

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“…Positive and flat power law surface density profiles (q = 0 and 1) for the inner disk of transition disks have previously been suggested by Dong et al (2012) in the framework of their general disk model to explain the H-band scattered light present inside the sub-mm dust cavities. Our results for the modeling of the CO ro-vibrational lines in HD 135344B provide an independent argument suggesting that the surface density profile inside the cavity can increase with radius in transition disks.…”

Section: Discussionmentioning

confidence: 80%

Constraining the structure of the transition disk HD 135344B (SAO 206462) by simultaneous modeling of multiwavelength gas and dust observations

Carmona

Pinte

Thi

et al. 2014

A&A

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Context. Constraining the gas and dust disk structure of transition disks, particularly in the inner dust cavity, is a crucial step toward understanding the link between them and planet formation. HD 135344B is an accreting (pre-)transition disk that displays the CO 4.7 µm emission extending tens of AU inside its 30 AU dust cavity. Aims. We constrain HD 135344B's disk structure from multi-instrument gas and dust observations. Methods. We used the dust radiative transfer code MCFOST and the thermochemical code ProDiMo to derive the disk structure from the simultaneous modeling of the spectral energy distribution (SED), VLT/CRIRES CO P(10) 4.75 µm, Herschel/PACS [O ] 63 µm, Spitzer/IRS, and JCMT 12 CO J = 3−2 spectra, VLTI/PIONIER H-band visibilities, and constraints from (sub-)mm continuum interferometry and near-IR imaging. Results. We found a disk model able to describe the current gas and dust observations simultaneously. This disk has the following structure. (1) To simultaneously reproduce the SED, the near-IR interferometry data, and the CO ro-vibrational emission, refractory grains (we suggest carbon) are present inside the silicate sublimation radius (0.08 < R < 0.2 AU). (2) The dust cavity (R < 30 AU) is filled with gas, the surface density of the gas inside the cavity must increase with radius to fit the CO ro-vibrational line profile, a small gap of a few AU in the gas distribution is compatible with current data, and a large gap of tens of AU in the gas does not appear likely. (4) The gas-to-dust ratio inside the cavity is >100 to account for the 870 µm continuum upper limit and the CO P(10) line flux.(5) The gas-to-dust ratio in the outer disk (30 < R < 200 AU) is <10 to simultaneously describe the [O ] 63 µm line flux and the CO P(10) line profile. (6) In the outer disk, most of the gas and dust mass should be located in the midplane, and a significant fraction of the dust should be in large grains. Conclusions. Simultaneous modeling of the gas and dust is required to break the model degeneracies and constrain the disk structure. An increasing gas surface density with radius in the inner cavity echoes the effect of a migrating jovian planet in the disk structure. The low gas mass (a few Jupiter masses) throughout the HD 135344B disk supports the idea that it is an evolved disk that has already lost a large portion of its mass.

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Section: Discussionmentioning

confidence: 80%

Constraining the structure of the transition disk HD 135344B (SAO 206462) by simultaneous modeling of multiwavelength gas and dust observations

Carmona

Pinte

Thi

et al. 2014

A&A

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“…′′ 15), the V4046 Sgr disk is a natural candidate to test this scenario with scattered light observations (e.g. Dong et al 2012).…”

Section: Discussionmentioning

confidence: 99%

THE STRUCTURE OF THE EVOLVED CIRCUMBINARY DISK AROUND V4046 Sgr

Rosenfeld

Andrews

Wilner

et al. 2013

ApJ

141

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We present sensitive, sub-arcsecond resolution Submillimeter Array observations of the protoplanetary disk around the nearby, pre-main sequence spectroscopic binary V4046 Sgr. We report for the first time a large inner hole (r = 29 AU) spatially resolved in the 1.3 mm continuum emission and study the structure of this disk using radiative transfer calculations to model the spectral energy distribution (SED), continuum visibilities, and spectral line emission of CO and its main isotopologues. Our modeling scheme demonstrates that the majority of the dust mass is distributed in a narrow ring (centered at 37 AU with a FWHM of 16 AU) that is ∼5× more compact than the gas disk. This structure implies that the dust-to-gas mass ratio has a strong spatial variation, ranging from a value much larger than typical of the interstellar medium (ISM) at the ring to much smaller than that of the ISM at larger disk radii. We suggest that these basic structural features are potentially observational signatures of the accumulation of solids at a local gas pressure maximum. These models also require a substantial population of ∼µm-sized grains inside the central disk cavity. We suggest that this structure is likely the result of dynamical interactions with a low-mass companion, although photoevaporation may also play a secondary role.Subject headings: circumstellar matter -protoplanetary disks -planet-disk interactions -submillimeter: planetary systems -stars: individual (V4046 Sgr)

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“…The anisotropic scattering phase function is approximated using the Henyey-Greenstein function (Henyey & Greenstein 1941). The optical properties can be found in Dong et al (2012, Figure 2). …”

Section: Hydrodynamic and Near-infrared Radiative Transfer Modelingmentioning

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

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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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The Missing Cavities in the Seeds Polarized Scattered Light Images of Transitional Protoplanetary Disks: A Generic Disk Model

Cited by 117 publications

References 57 publications

Constraining the structure of the transition disk HD 135344B (SAO 206462) by simultaneous modeling of multiwavelength gas and dust observations

Constraining the structure of the transition disk HD 135344B (SAO 206462) by simultaneous modeling of multiwavelength gas and dust observations

THE STRUCTURE OF THE EVOLVED CIRCUMBINARY DISK AROUND V4046 Sgr

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

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