DUST PROPERTIES AND DISK STRUCTURE OF EVOLVED PROTOPLANETARY DISKS IN Cep OB2: GRAIN GROWTH, SETTLING, GAS AND DUST MASS, AND INSIDE-OUT EVOLUTION

Sicilia‐Aguilar, A.; Henning, Thomas; Dullemond, C. P.; Patel, Nimesh; Juhász, A.; Bouwman, J.; Sturm, B.

doi:10.1088/0004-637x/742/1/39

Cited by 32 publications

(42 citation statements)

References 103 publications

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“…The used material is quartz dust with a grain size distribution between 0.5 µm and 10 µm with 80% of the mass between 1 µm and 5 µm. This is in good agreement with grain sizes predicted for protoplanetary disks (Sicilia-Aguilar et al 2011).…”

Section: Methodssupporting

confidence: 91%

Evolution of macroscopic dust agglomerates – Implications for planetesimal growth

Teiser

Engelhardt

Küpper

et al. 2012

EAS Publications Series

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Abstract. The formation of preplanetary bodies is studied in laboratory experiments, especially the growth of decimeter bodies. As these macroscopic bodies are the building blocks for many growth models, it is very important to investigate possible formation processes and the mechanical properties of large dust agglomerates. Here, experimental results on the properties of decimeter-sized dust agglomerates and results of impact experiments at large collision velocities are presented. Fragmentation is a key process to growth at high velocities as energy is dissipated. Growth is observed for velocities up to 56 m/s and impact angles of up to 45 • .

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Section: Methodssupporting

confidence: 91%

Evolution of macroscopic dust agglomerates – Implications for planetesimal growth

Teiser

Engelhardt

Küpper

et al. 2012

EAS Publications Series

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“…It is also the only disk with confirmed accretion in this 12 Myr-old cluster, and one of the strongest accretors among low-mass stars in the whole Cep OB2 region (Ṁ = 4 +3 −2 × 10 −8 M /yr; Sicilia-Aguilar et al 2010). Remarkably, its mid-IR flux is relatively modest compared to similar objects in Tr 37, which had been previously interpreted as a lack of small dust in the disk (Sicilia-Aguilar et al 2011). The object is clearly detected at 70 µm, but not at 160 µm.…”

Section: Low Far-ir Flux In a Strongly Accreting Star: 11-2037mentioning

confidence: 69%

“…This is not observed at significant levels. Variations in the disk vertical structure (flaring/thickness) are common in disks (Sicilia-Aguilar et al 2011) and can affect α(H-70 µm), washing out potential correlations between the 70 µm fluxes and the accretion rate. There is also the possibility that the various physical conditions (or grain properties) throughout the disk affect the viscosity and thus the global viscous transport (Isella et al 2009).…”

Section: Discussionmentioning

confidence: 99%

“…The K4.5 star 11-2037 has a remarkable low 70 µm flux for its Spitzer fluxes and its IRAM/1.3 mm detection (Sicilia-Aguilar et al 2011). This is an example where our previous disk models fail to predict the observed Herschel fluxes, which are lower The colour lines show models with different vertical structures (flaring laws H/R, outer disk thickness), grain size distributions, and disk masses.…”

Section: Low Far-ir Flux In a Strongly Accreting Star: 11-2037mentioning

confidence: 92%

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TheHerschel/PACS view of the Cep OB2 region: Global protoplanetary disk evolution and clumpy star formation

Sicilia‐Aguilar

Roccatagliata

Getman

et al. 2014

A&A

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Context. The Cep OB2 region, with its two intermediate-aged clusters Tr 37 and NGC 7160, is a paradigm of sequential star formation and an ideal site for studies of protoplanetary disk evolution. Aims. We use Herschel data to study the protoplanetary disks and the star formation history of the region. Methods. Herschel/PACS observations at 70 and 160 µm probe the disk properties (mass, dust sizes, structure) and the evolutionary state of a large number of young stars. Far-IR data also trace the remnant cloud material and small-scale cloud structure. Results. We detect 95 protoplanetary disks at 70 µm, 41 at 160 µm, and obtain upper limits for more than 130 objects. The detection fraction at 70 µm depends on the spectral type (88% for K4 or earlier stars, 17% for M3 or later stars) and on the disk type (∼50% for full and pre-transitional disks, ∼35% for transitional disks, no low-excess/depleted disks detected). Non-accreting disks are not detected, suggesting significantly lower masses. Accreting transition and pre-transition disks have systematically higher 70 µm excesses than full disks, suggestive of more massive, flared and/or thicker disks. Herschel data also reveal several mini-clusters in Tr 37, which are small, compact structures containing a few young stars surrounded by nebulosity. Conclusions. Far-IR data are an excellent probe of the evolution of disks that are too faint for sub-millimetre observations. We find a strong link between far-IR emission and accretion, and between the inner and outer disk structure. Herschel confirms the dichotomy between accreting and non-accreting transition disks. Accretion is a powerful measure of global disk evolution: substantial mass depletion and global evolution need to occur to shut down accretion in a protoplanetary disk, even if the disk has inner holes. Disks likely follow different evolutionary paths: low disk masses do not imply opening inner holes, and having inner holes does not require low disk masses. The mini-clusters reveal multi-episodic star formation in Tr 37. The long survival of mini-clusters suggest that they formed from the fragmentation of the same core. Their various morphologies favour different formation/triggering mechanisms acting within the same cluster. The beads-on-a-string structure in one mini-cluster is consistent with gravitational fragmentation or gravitational focusing, acting on very small scales (solar-mass stars in ∼0.5 pc filaments). Multi-episodic star formation could also produce evolutionary variations between disks in the same region. Finally, Herschel also unveils what could be the first heavy mass loss episode of the O6.5 star HD 206267 in Tr 37.

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“…Only when no reasonable fit to the observed SED could be achieved with the simplified models, we included additional parameters, specifically by considering inclusion of large grains/removal of small grains in the dust component, modification of the inner disk rim to include an inner hole at distances larger than the dust destruction radius, and variation of the flaring and dust properties between the inner and outer disk. This is the same procedure as the one we followed for the disks in Cep OB2 (Sicilia-Aguilar et al 2011b). The properties of the best-fitting models are listed in Table 6.…”

Section: Disk Properties In the Coronet Clustermentioning

confidence: 99%

Protostars, multiplicity, and disk evolution in the Corona Australis region: aHerschelGould Belt Study

Sicilia‐Aguilar

Henning

Linz

et al. 2013

A&A

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Context. The CrA region and the Coronet cluster form a nearby (138 pc), young (1−2 Myr) star-forming region that hosts a moderate population of Class I, II, and III objects. Aims. We study the structure of the cluster and the properties of the protostars and protoplanetary disks in the region. Methods. We present Herschel PACS photometry at 100 and 160 μm, obtained as part of the Herschel Gould Belt Survey. The Herschel maps reveal the cluster members within the cloud with high sensitivity and high dynamic range. Results. Many of the cluster members are detected, including some embedded, very low-mass objects, several protostars (some of them extended), and substantial emission from the surrounding molecular cloud. Herschel also reveals some striking structures, such as bright filaments around the IRS 5 protostar complex and a bubble-shaped rim associated with the Class I object IRS 2. The disks around the Class II objects display a wide range of mid-and far-IR excesses consistent with different disk structures. We have modeled the disks with the RADMC radiative transfer code to quantify their properties. Some of them are consistent with flared, massive, relatively primordial disks (S CrA, T CrA). Others display significant evidence for inside-out evolution, consistent with the presence of inner holes/gaps (G-85, G-87). Finally, we found disks with a dramatic small dust depletion (G-1, HBC 677) that, in some cases, could be related to truncation or to the presence of large gaps in a flared disk (CrA-159). The derived masses for the disks around the low-mass stars are found to be below the typical values in Taurus, in agreement with previous Spitzer observations. Conclusions. The Coronet cluster presents itself as an interesting compact region that contains both young protostars and very evolved disks. The Herschel data provide sufficient spatial resolution to detect small-scale details, such as filamentary structures or spiral arms associated with multiple star formation. The disks around the cluster members range from massive, flared primordial disks to disks with substantial small dust grain depletion or with evidence of inside-out evolution. This results in an interesting mixture of objects for a young and presumably coevally formed cluster. Given the high degree of multiplicity and interactions observed among the protostars in the region, the diversity of disks may be a consequence of the early star formation history, which should also be taken into account when studying the disk properties in similar sparsely populated clusters.

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DUST PROPERTIES AND DISK STRUCTURE OF EVOLVED PROTOPLANETARY DISKS IN Cep OB2: GRAIN GROWTH, SETTLING, GAS AND DUST MASS, AND INSIDE-OUT EVOLUTION

Cited by 32 publications

References 103 publications

Evolution of macroscopic dust agglomerates – Implications for planetesimal growth

Evolution of macroscopic dust agglomerates – Implications for planetesimal growth

TheHerschel/PACS view of the Cep OB2 region: Global protoplanetary disk evolution and clumpy star formation

Protostars, multiplicity, and disk evolution in the Corona Australis region: aHerschelGould Belt Study

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