Gas- and dust evolution in protoplanetary disks

By T. Birnstiel, C. Dullemond, F. Brauer. 2010

459 citations recorded by the source corpus.

Context. Current models of the size- and radial evolution of dust in protoplanetary disks generally oversimplify either the radial evolution of the disk (by focussing at one single radius or by using steady state disk models) or they assume particle growth to proceed monodispersely or without fragmentation. Further studies of protoplanetary disks - such as observations, disk chemistry and structure calculations or planet population synthesis models - depend on the distribution of dust as a function of grain size and radial position in the disk. Aims. We attempt to improve upon current models to be able to investigate how the initial conditions, the build-up phase, and the evolution of the protoplanetary disk influence growth and transport of dust. Methods. We introduce a new model similar to Brauer et al. (2008, A&A, 480, 859) in which we now include the time-dependent viscous evolution of the gas disk, and in which more advanced input physics and numerical integration methods are implemented. Results. We show that grain properties, the gas pressure gradient, and the amount of turbulence are much more influencing the evolution of dust than the initial conditions or the build-up phase of the protoplanetary disk. We quantify which conditions or environments are favorable for growth beyond the meter size barrier. High gas surface densities or zonal flows may help to overcome the problem of radial drift, however already a small amount of turbulence poses a much stronger obstacle for grain growth.

Subfields: Astronomy and Astrophysics, Fluid Flow and Transfer Processes, Spectroscopy

View Paper: https://www.semanticscholar.org/paper/5709a9d50539c8f271a1fda9cdaf925684e65c4d

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Fluid Flow and Transfer Processes

In Spectroscopy

Citations in the corpus

Dust size distributions in coagulation/fragmentation equilibrium: numerical solutions and analytical fits (2010, methodology): “In this section, we will test the analytical predictions of the previous section by a coagulation/fragmentation code (Birnstiel et al. 2010a; see also Brauer et al. 2008a).”
Trapping dust particles in the outer regions of protoplanetary disks (2011, methodology): “Note also that the match between the model presented here with A = 0.3 is better than what has been obtained by Birnstiel et al. (2010b).”
Photodissociation and photoionisation of atoms and molecules of astrophysical interest (2017, background): “This phenomena is observed (e.g., Li & Lunine 2003; Kessler-Silacci et al. 2006; Testi et al. 2014) and predicted (e.g., Birnstiel et al. 2010) to occur in protoplanetary disks, at least up to cm-sized grains, with the larger grains settling to the midplane and drifting towards the central star.”
Astrochemistry and compositions of planetary systems (2020, background): “Thus water ice coated grains are expected to readily grow to pebble sizes beyond the water snowline, while growth may be limited to sub-cm sizes in the innermost disk regions (Birnstiel et al. 2010).”
Planetesimal formation by sweep-up: how the bouncing barrier can be beneficial to growth (2012, methodology): “At these large collision energies, the particles tend to fragment rather thanstick (Blum & Wurm 2008), which effectively prevents further growth (Dullemond & Dominik 2005; Brauer et al. 2008; Birnstiel et al. 2010).”
Multiple Disk Gaps and Rings Generated by a Single Super-Earth (2017, methodology): “Big dust particles, having sizes s = 0.2 mm as in the hydro simulations, are assumed to have settled to the disk midplane (e.g., Dullemond & Dominik 2004; Birnstiel et al. 2010).”
Dust Evolution and the Formation of Planetesimals (2016, background): “Moreover, for a conversion from the (sub-)millimeter fluxes into disk masses, one needs to know the gas-to-dust ratio, which is expected to change with disk radii and with disk evolution (Takeuchi & Lin 2002; Birnstiel et al. 2010).”
A simple model for the evolution of the dust population in protoplanetary disks (2012, methodology): “A detailed description of the model can be found in Birnstiel et al. (2010).”
Small vs. large dust grains in transitional disks: do different cavity sizes indicate a planet? - SAO 206462 (HD 135344B) in polarized light with VLT/NACO (2013, methodology): “To show this, we calculate the Stokes number St, defined as: St(a,R) = ρS(R) · a Σg(R) · π 2 (3) (Birnstiel et al. 2010) wherea is the particle size,ρS the solid density of dust particles, andΣg the gas column density.”
The Disk Substructures at High Angular Resolution Project (DSHARP). VI. Dust Trapping in Thin-ringed Protoplanetary Disks (2018, methodology): “D effects, full radiative transfer (e.g. Bitsch et al. 2013; Flock et al. 2013), dust growth and fragmentation (e.g. Birnstiel et al. 2010; Okuzumi et al. 2012), and many other things.”
The VLA/ALMA Nascent Disk and Multiplicity (VANDAM) Survey of Orion Protostars. II. A Statistical Characterization of Class 0 and Class I Protostellar Disks (2020, background): “Simulations have shown that rapid dust growth and radial drift are possible in protostellar disks (Birnstiel et al. 2010), subsequently affecting the apparent radius measured from dust emission.”
Multiwavelength analysis for interferometric (sub-)mm observations of protoplanetary disks - Radial constraints on the dust properties and the disk structure (2015, background): “In the recent theoretical studies by Brauer et al. (2008) and Birnstiel et al. (2010) the evolution of dust grain populations have been modeled taking into account dust growth processes (coagulation and fragmentation) and the dynamical mechanisms responsible for the transport of dust grains (radial…”
Survival of molecular gas in cavities of transition disks - I. CO (2013, methodology): “In a forthcoming paper, we plan to couple the present model with a model for dust evolution (Birnstiel et al. 2010, 2011, 2012b) which will allow us to study the combined use of lines and the continuum in order to better constrain the gap formation mechanism.”
Dust grain growth in ρ-Ophiuchi protoplanetary disks (2010, background): “Birnstiel et al. (2010b) have compared the observed fluxes at millimeter wavelengths for the disks samples described in R10 and in this paper with predictions of dust evolution models accounting for coagulation and fragmentation.”
Breaking through: The effects of a velocity distribution on barriers to dust growth (2012, methodology): “We implement a Maxwellian velocity distribution together with three simple collisions models into a local version of the dustsize evolution code of Birnstiel et al. (2010).”
THE MASS AND SIZE DISTRIBUTION OF PLANETESIMALS FORMED BY THE STREAMING INSTABILITY. I. THE ROLE OF SELF-GRAVITY (2015, background): “2 ing shows that particles within this size range do not easily stick together, and instead fragment or bounce (Brauer et al. 2008; Blum & Wurm 2008; Birnstiel et al. 2010; Zsom et al. 2010).”
RESOLVED IMAGES OF LARGE CAVITIES IN PROTOPLANETARY TRANSITION DISKS (2011, background): “For example, models of the grain size evolution in disks predict smooth κ variations (Dullemond & Dominik 2005; Garaud 2007; Brauer et al. 2008; Birnstiel et al. 2010), rather than the abrupt optical depth change near Rcav that is observed.”