PRE-TRANSITIONAL DISK NATURE OF THE AB Aur DISK

Honda, Mitsuhiko; Inoue, Akio; Okamoto, Y.; Kataza, Hirokazu; Fukagawa, Misato; Yamashita, Takuya; Fujiyoshi, Takuya; Tamura, Motohide; Hashimoto, Jun; Miyata, Takashi; Sako, Shigeyuki; Sakon, Itsuki; Fujiwara, Hideo; Kamizuka, Takafumi; Onaka, Takashi

doi:10.1088/2041-8205/718/2/l199

Cited by 17 publications

(23 citation statements)

References 41 publications

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“…In addition, the HiCIAO images show a radial gap at ∼80 AU clearly seen in the northern direction as well as the inner emission near the mask edge. Note that the location of the outer ring outside of the gap is consistent with the disk wall inferred from the mid-infrared and submillimeter thermal imaging (Honda et al 2010). The observed fine and irregular structure may favor planets in the disk.…”

Section: Imaging Polarimetry With Subaru/hiciaosupporting

confidence: 79%

High-contrast polarimetric imaging of the protoplanetary disk around AB Aurigae

et al. 2010

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Abstract. We present the spatially-resolved polarization measurements for the disk around the Herbig Ae star, AB Aurigae. The images were obtained in J , H, and Ks bands with the coronagraphic camera HiCIAO on the Subaru Telescope. The inner region beyond 30 AU from the star was imaged, which reveals an azimuthal dip, a radial gap at around 80 AU, and complex spiral-like emission in polarized light.

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Section: Imaging Polarimetry With Subaru/hiciaosupporting

confidence: 79%

High-contrast polarimetric imaging of the protoplanetary disk around AB Aurigae

et al. 2010

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“…These data also revealed an approximately 16 au wide gap in the disk. Centered at 80 au from the central star, it is similar to the mid-IR gap inferred by Honda et al (2010) from models of their 24.6 μm imagery, but appears to be different from the gap detected by Tang et al (2012), who found a gap that ends at approximately 110 au and is about 90 au wide in 1.3 mm continuum emission.…”

Section: Introductionsupporting

confidence: 44%

Constraining the Movement of the Spiral Features and the Locations of Planetary Bodies Within the Ab Aur System

Lomax

Wisniewski

Grady

et al. 2016

ApJ

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We present a new analysis of multi-epoch, H-band, scattered light images of the AB Aur system. We use a Monte Carlo radiative transfer code to simultaneously model the system's spectral energy distribution (SED) and H-band polarized intensity (PI) imagery. We find that a disk-dominated model, as opposed to one that is envelopedominated, can plausibly reproduce AB Aur's SED and near-IR imagery. This is consistent with previous modeling attempts presented in the literature and supports the idea that at least a subset of AB Aur's spirals originate within the disk. In light of this, we also analyzed the movement of spiral structures in multi-epoch H-band total light and PI imagery of the disk. We detect no significant rotation or change in spatial location of the spiral structures in these data, which span a 5.8-year baseline. If such structures are caused by disk-planet interactions, the lack of observed rotation constrains the location of the orbit of planetary perturbers to be >47 au.

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“…Alternatively, the amorphous silicate feature may originate in the inner disk. Examples are HD 142527 (Verhoeff et al 2011), AB AUr (Honda et al 2010), and HD 36112 (Isella et al 2010). In these objects large dust gaps of several tens of AUs have also been found.…”

Section: Discussionmentioning

confidence: 98%

Large dust gaps in the transitional disks of HD 100453 and HD 34282

Khalafinejad

Maaskant

Mariñas

et al. 2016

A&A

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Context. The formation of dust gaps in protoplanetary disks is one of the most important signs of disk evolution and might indicate the formation of planets. Aims. We aim to characterize the flaring disk structure around the Herbig Ae/Be stars HD 100453 and HD 34282. Their spectral energy distributions (SEDs) show an emission excess between 15−40 µm, but very weak (HD 100453) and no (HD 34282) signs of the 10 and 20 µm amorphous silicate features. We investigate whether this implies the presence of large dust gaps. Methods. We investigated spatially resolved mid-infrared Q-band images taken with Gemini North/MICHELLE. We performed radiative transfer modeling and examined the radial distribution of dust. We simultaneously fit the Q-band images and SEDs of HD 100453 and HD 34282. Results. Our solutions require that the inner halos and outer disks be separated by large dust gaps that are depleted with respect to the outer disk by a factor of 1000 or more. The inner edges of the outer disks of HD 100453 and HD 34282 have temperatures of ∼160 ± 10 K and ∼60 ± 5 K, respectively. Because of the high surface brightness of these walls, they dominate the emission in the Q band. Their radii are constrained at 20 +2 −2 AU and 92 +31 −17 AU, respectively. Conclusions. HD 100453 and HD 34282 most likely have disk dust gaps. The upper limit of the dust mass in each gap is estimated to be about 10 −7 M . We find that the locations and sizes of disk dust gaps are connected to the SED, as traced by the mid-infrared flux ratio F 30 /F 13.5 . We propose a new classification scheme for the Meeus groups based on the F 30 /F 13.5 ratio. The absence of amorphous silicate features in the observed SEDs is caused by the depletion of small ( 1 µm) silicate dust at temperatures above 160 K, which could be related to the presence of a dust gap in that region of the disk.

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PRE-TRANSITIONAL DISK NATURE OF THE AB Aur DISK

Cited by 17 publications

References 41 publications

High-contrast polarimetric imaging of the protoplanetary disk around AB Aurigae

High-contrast polarimetric imaging of the protoplanetary disk around AB Aurigae

Constraining the Movement of the Spiral Features and the Locations of Planetary Bodies Within the Ab Aur System

Large dust gaps in the transitional disks of HD 100453 and HD 34282

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