Testing the theory of grain growth and fragmentation by millimeter observations of protoplanetary disks

Birnstiel, T.; Ricci, Luca; Trotta, Francesco; Dullemond, C. P.; Natta, A.; Testi, L.; Dominik, C.; Henning, Thomas; Ormel, Chris W.; Zsom, Andras

doi:10.1051/0004-6361/201014893

Cited by 112 publications

(131 citation statements)

References 32 publications

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“…local pressure maxima due to turbulent vortices or spiral density waves, have been invoked. Birnstiel et al (2010b) have compared the observed fluxes at millimeter wavelengths for the disks samples described in R10 and in this paper with Fig. 7.…”

Section: Grain Growthmentioning

confidence: 96%

“…The observed flux of the fainter disks are instead typically overpredicted even by more than one order of magnitude. These discrepancies may be explained by considering in the disk models a dust reduction due to radial drift at a reduced rate 14 or during an earlier evolutionary time or due to efficient conversion of dust into larger, unseen bodies (see Birnstiel et al 2010b for more details). Observations of these faint disks can thus help us to determine which mechanisms play a major role for the dynamics and evolution of large grains in the outer regions of disks.…”

Section: Grain Growthmentioning

confidence: 99%

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Dust grain growth inρ-Ophiuchi protoplanetary disks

Ricci¹,

Testi²,

Natta

et al. 2010

A&A

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212

140

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We present new ATCA observations at 3.3 mm of 27 young stellar objects in the ρ-Oph young cluster. 25 of these sources have been detected. We analyze the sub-millimeter and millimeter SED for a subsample of 17 isolated class II protoplanetary disks and derive constraints on the grain growth and total dust mass in the disk outer regions. All the disks in our sample show a mm slope of the SED which is significantly shallower than the one observed for the ISM at these long wavelengths. This indicates that 1) class II disks in Ophiuchus host grains grown to mm/cm-sizes in their outer regions; 2) formation of mm/cm-sized pebbles is a fast process and 3) a mechanism halting or slowing down the inward radial drift of solid particles is required to explain the data. These findings are consistent with previous results in other star forming regions. We compare the dust properties of this sample with those of a uniformly selected sample in Taurus-Auriga and find no statistical evidence of any difference in terms of grain growth between the two regions. Finally, in our sample the mm slope of the SED is not found to correlate with indicators of grain growth to micron sizes in the surface layers of the inner disk.

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Section: Grain Growthmentioning

confidence: 96%

Section: Grain Growthmentioning

confidence: 99%

Dust grain growth inρ-Ophiuchi protoplanetary disks

Ricci¹,

Testi²,

Natta

et al. 2010

A&A

Self Cite

212

140

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show abstract

“…Scattered light images of the circumstellar disk surrounding the T Tauri star IM Lupi may indicate the presence of fluffy aggregates (Pinte et al 2008). Birnstiel et al (2010) and Ricci et al (2010Ricci et al ( , 2012 used porous spherical grains to specify the dust opacity in a sample of young protoplanetary disks. For a general study of the influence of porosity on the dust opacity in protoplanetary disks, see Semenov et al (2003).…”

Section: Introductionmentioning

confidence: 99%

Porous dust grains in debris disks

Kirchschlager

Wolf

2013

A&A

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Aims. When modeling the density and grain size distribution in debris disks, the minimum particle size is often significantly larger than the corresponding blowout size. While the dust particles are usually modeled as compact, homogenous spheres, we instead investigate the impact of porosity. The optical properties of porous particles are determined, and the influences of porosity on the blowout size and dust temperatures investigated. Methods. Using the method of discrete dipole approximation, we calculate the scattering and absorption cross sections of porous particles and derive the blowout size and the behavior of the dust temperature. Results. We determine the efficiency factors of absorption and the radiation pressure for porous particles, and investigate the influence on the β-ratio. Blowout sizes are calculated for various stellar luminosities and porosities, and an approximation equation is derived to estimate the blowout size as a function of these parameters. Furthermore, we investigate the influence of the porosity on the dust equilibrium temperature. Conclusions. The blowout size increases with the particle porosity and stellar luminosity. The dust temperature of porous particles is lower than the one of the compact spheres; in particular, the temperature of blowout grains decreases for porous particles.

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“…It also implies that pebbles are constantly replenished: they are lost to the inner disk, but drift in from the outer disk. Pebble accretion, in contrast to planetesimal accretion, is therefore a global phenomenon: one has to consider the evolution of the dust population throughout the entire disk (Birnstiel et al 2010;Okuzumi et al 2012;Testi et al 2014). …”

Section: Pebblesmentioning

confidence: 99%

The Emerging Paradigm of Pebble Accretion

Ormel

2017

Astrophysics and Space Science Library

113

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Pebble accretion is the mechanism in which small particles ("pebbles") accrete onto big bodies (planetesimals or planetary embryos) in gas-rich environments. In pebble accretion, accretion occurs by settling and depends only on the mass of the gravitating body, not its radius. I give the conditions under which pebble accretion operates and show that the collisional cross section can become much larger than in the gas-free, ballistic, limit. In particular, pebble accretion requires the pre-existence of a massive planetesimal seed. When pebbles experience strong orbital decay by drift motions or are stirred by turbulence, the accretion efficiency is low and a great number of pebbles are needed to form Earth-mass cores. Pebble accretion is in many ways a more natural and versatile process than the classical, planetesimal-driven paradigm, opening up avenues to understand planet formation in solar and exoplanetary systems.

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Testing the theory of grain growth and fragmentation by millimeter observations of protoplanetary disks

Cited by 112 publications

References 32 publications

Dust grain growth inρ-Ophiuchi protoplanetary disks

Dust grain growth inρ-Ophiuchi protoplanetary disks

Porous dust grains in debris disks

The Emerging Paradigm of Pebble Accretion

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