Hd 100453: A Link Between Gas-Rich Protoplanetary Disks and Gas-Poor Debris Disks

Collins, Karen A.; Grady, C. A.; Hamaguchi, Kenji; Wisniewski, John P.; Brittain, S.; Sitko, Michael L.; Carpenter, W. J.; Williams, Jonathan P.; Mathews, Geoffrey S.; Williger, G. M.; Boekel, R. van; Henning, Th.; Ancker, M. E. van den; Meeus, G.; Chen, X. P.; Petre, Robert; Woodgate, B. E.

doi:10.1088/0004-637x/697/1/557

Cited by 46 publications

(78 citation statements)

References 90 publications

(101 reference statements)

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“…The first measurement was obtained with VLT/NACO in 2003 under program ID: 071.C-0507 (PI: Mouillet) and presented in Chen et al (2006). These data were reprocessed, along with an additional epoch from the same telescope/instrument in 2006 (program ID: 077.C-0570, PI: van Boekel) and presented in Collins et al (2009). We utilize these published separation and position angle (PA) measurements in our astrometric catalog (see Section 5.1) and refer interested readers to these respective publications for the details of the data acquisition and processing.…”

Section: Published Vlt/naco Datamentioning

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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Section: Published Vlt/naco Datamentioning

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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“…Two early-type disks lie below even the late-type locus on the CO 6−5 axis. Two of these resemble debris disks: HD 141569 is a transitional disk with no substantial surface density at radii below ∼95 au (Dent et al 2005;Jonkheid et al 2006), and HD 100453 has a CO-based gas mass of only 10 −4 M and an inner cavity of 20 au (Khalafinejad et al 2016;Collins et al 2009). …”

Section: Herbig Ae/be Systems (Spectral Types B a F)mentioning

confidence: 99%

Observations and modelling of CO and [C i] in protoplanetary disks

Kama

Bruderer

Carney

et al. 2016

A&A

111

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Context. The gas-solid budget of carbon in protoplanetary disks is related to the composition of the cores and atmospheres of the planets forming in them. The principal gas-phase carbon carriers CO, C 0 , and C + can now be observed regularly in disks. Aims. The gas-phase carbon abundance in disks has thus far not been well characterized observationally. We obtain new constraints on the [C]/[H] ratio in a large sample of disks, and compile an overview of the strength of [C ] and warm CO emission. Methods. We carried out a survey of the CO 6-5 line and the [C ] 1-0 and 2-1 lines towards 37 disks with the APEX telescope, and supplemented it with [C ] data from the literature. The data are interpreted using a grid of models produced with the DALI disk code.We also investigate how well the gas-phase carbon abundance can be determined in light of parameter uncertainties.

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“…HD 100453 is thought to be in transition between a gas-rich protoplanetary disk and a gas-poor debris disk (Collins et al 2009). Observations of spatially resolved Q-band imaging (Mariñas et al 2011), the SED, and the absence of the silicate feature are indications of a dust gap Maaskant et al (2013).…”

Section: Hd 100453mentioning

confidence: 99%

“…Observations of spatially resolved Q-band imaging (Mariñas et al 2011), the SED, and the absence of the silicate feature are indications of a dust gap Maaskant et al (2013). HD 100453 has a close M-type companion (projected distance of 120 AU), and the connection of the companion with the disk structure is not well understood (Collins et al 2009). Collins et al (2009) presented two non-detections.…”

Section: Hd 100453mentioning

confidence: 99%

“…HD 100453 has a close M-type companion (projected distance of 120 AU), and the connection of the companion with the disk structure is not well understood (Collins et al 2009). Collins et al (2009) presented two non-detections. The first one is CO 4.97 µm ro-vibrational emission with Gemini/Pheonix (these transitions trace hot and warm gas), and the second one is CO 3-2 rotational emission with JCMT/HARP at 867 micron (this is a coldgas tracer).…”

Section: Hd 100453mentioning

confidence: 99%

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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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Hd 100453: A Link Between Gas-Rich Protoplanetary Disks and Gas-Poor Debris Disks

Cited by 46 publications

References 90 publications

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

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

Observations and modelling of CO and [C i] in protoplanetary disks

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

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