Dust grain growth in<i>ρ</i>-Ophiuchi protoplanetary disks

Ricci, Luca; Testi, L.; Natta, A.; Brooks, Kate

doi:10.1051/0004-6361/201015039

Cited by 212 publications

(150 citation statements)

References 45 publications

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“…7, our model images are very similar to the transition disks observations in the (sub-)millimeter regime, that reveal a continuum emission as a resolved ring-like feature (e.g., Williams & Cieza 2011;Andrews et al 2011a;Isella et al 2012). In addition, after 1 Myr of dust evolution, we estimate a spectral index of ∼2.7 by integrating the flux over the entire disk at wavelengths of 1 mm (Ricci et al 2010).…”

Section: Emission Mapssupporting

confidence: 79%

“…In addition, high relative velocities lead to numerous fragmentation collisions converting a large object into smaller dust particles. The same physical process happens to the millimeter-size particles that are observed in the outer regions of the disk (e.g., Wilner et al 2000;Ricci et al 2010;Guilloteau et al 2011). One possible solution to prevent the rapid inward drift and trap dust particles is to consider pressure bumps (Klahr & Henning 1997;Fromang & Nelson 2005;Brauer et al 2008;Johansen et al 2009;Pinilla et al 2012).…”

Section: Introductionmentioning

confidence: 98%

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Ring shaped dust accumulation in transition disks

Pinilla¹,

Benisty²,

Birnstiel³

2012

A&A

406

535

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Context. Transition disks are believed to be the final stages of protoplanetary disks, during which a forming planetary system or photoevaporation processes open a gap in the inner disk, drastically changing the disk structure. From theoretical arguments it is expected that dust growth, fragmentation and radial drift are strongly influenced by gas disk structure, and pressure bumps in disks have been suggested as key features that may allow grains to converge and grow efficiently. Aims. We want to study how the presence of a large planet in a disk influences the growth and radial distribution of dust grains, and how observable properties are linked to the mass of the planet. Methods. We combined two-dimensional hydrodynamical disk simulations of disk-planet interactions with state-of-the-art coagulation/fragmentation models to simulate the evolution of dust in a disk, which has a gap created by a massive planet. We computed images at different wavelengths and illustrated our results using the example of the transition disk LkCa15. Results. The gap opened by a planet and the long-range interaction between the planet and the outer disk create a single large pressure bump outside the planetary orbit. Millimeter-sized particles form and accumulate at the pressure maximum and naturally produce ring-shaped sub-millimeter emission that is long-lived because radial drift no longer depletes the large grain population of the disk. For large planet masses around 9 M Jup , the pressure maximum and, therefore, the ring of millimeter particles is located at distances that can be more than twice the star-planet separation, creating a large spatial separation between the gas inner edge of the outer disk and the peak millimeter emission. Smaller grains do get closer to the gap and we predict how the surface brightness varies at different wavelengths.

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Section: Emission Mapssupporting

confidence: 79%

Section: Introductionmentioning

confidence: 98%

Ring shaped dust accumulation in transition disks

Pinilla¹,

Benisty²,

Birnstiel³

2012

A&A

406

535

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“…It is found that, despite the young age of the cluster (∼1 Myr), many circumstellar disks in ρ Oph are evolved showing features such as millimeter size dust grains in the outer disk region (Furlan et al 2009;Andrews et al 2010;Ricci et al 2010), inner opacity holes characteristic of transition disks (Cieza et al 2010), dust settling, and dust grain processing (e.g., McClure et al 2010). In this section, and in light of the newly discovered substellar members in our survey, we use SEDs to classify the evolutionary state of each object.…”

Section: Slopes Of the Spectral Energy Distributionsmentioning

confidence: 99%

Spectroscopy of new brown dwarf members ofρ Ophiuchi and an updated initial mass function

Oliveira¹,

Moraux²,

Bouvier³

et al. 2012

A&A

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Aims. To investigate the universality hypothesis of the initial mass function in the substellar regime, the population of the ρ Ophiuchi molecular cloud is analysed by including a new sample of low-mass spectroscopically confirmed members. To that end, we have conducted a large spectroscopic follow-up of young substellar candidates uncovered in our previous photometric survey. Methods. The spectral types and extinction were derived for a newly found population of substellar objects, and its masses estimated by comparison to evolutionary models. A thoroughly literature search was conducted to provide an up-to-date census of the cluster, which was then used to derive the luminosity and mass functions, as well as the ratio of brown dwarfs to stars in the cluster. These results were then compared to other young clusters. Results. It is shown that the study of the substellar population of the ρ Ophiuchi molecular cloud is hampered only by the high extinction in the cluster ruling out an apparent paucity of brown dwarfs. The discovery of 16 new members of ρ Ophiuchi, 13 of them in the substellar regime, reveals the low-mass end of its population and shows the success of our photometric candidate selection with the WIRCam survey. The study of the brown dwarf population of the cluster reveals a high disk fraction of 76 +5 −8 %. Conclusions. Taking the characteristic peak mass of the derived mass function and the ratio of brown dwarfs to stars into account, we conclude that the mass function of ρ Ophiuchi is similar to other nearby young clusters.

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“…The grain size in protoplanetary disks has been constrained with the spectral index of the dust opacity coefficient at millimeter wavelengths (e.g., Beckwith et al 1990;Beckwith & Sargent 1991;Miyake & Nakagawa 1993;Andrews & Williams 2005;Isella et al 2009;Ricci et al 2010aRicci et al , 2010bvan der Marel et al 2013). The opacity index at millimeter wavelengths in protoplanetary disks has been shown to be as low as 0-1, which indicates that the grain size in protoplanetary disks is of the order of a millimeter or larger (e.g., Draine 2006).…”

Section: Introductionmentioning

confidence: 99%

Grain Size Constraints on Hl Tau With Polarization Signature

Kataoka

Muto

Momose

et al. 2016

ApJ

119

147

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The millimeter-wave polarization of the protoplanetary disk around HL Tau has been interpreted as the emission from elongated dust grains aligned with the magnetic field in the disk. However, the self-scattering of thermal dust emission may also explain the observed millimeter-wave polarization. In this paper, we report a modeling of the millimeter-wave polarization of the HL Tau disk with the self-polarization. Dust grains are assumed to be spherical and to have a power-law size distribution. We change the maximum grain size with a fixed dust composition in a fixed disk model to find the grain size to reproduce the observed signature. We find that the direction of the polarization vectors and the polarization degree can be explained with the self-scattering. Moreover, the polarization degree can be explained only if the maximum grain size is ∼150 μm. The obtained grain size from the polarization is different from that which has been previously expected from the spectral index of the dust opacity coefficient (a millimeter or larger) if the emission is optically thin. We discuss that porous dust aggregates may solve the inconsistency of the maximum grain size between the two constraints.

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Dust grain growth inρ-Ophiuchi protoplanetary disks

Cited by 212 publications

References 45 publications

Ring shaped dust accumulation in transition disks

Ring shaped dust accumulation in transition disks

Spectroscopy of new brown dwarf members ofρ Ophiuchi and an updated initial mass function

Grain Size Constraints on Hl Tau With Polarization Signature

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