An Analytical Model of Radial Dust Trapping in Protoplanetary Disks

Anibal Sierra1, Susana Lizano1, Enrique Macías2, Carlos Carrasco-González1, Mayra Osorio3, and Mario Flock4
Astrophysical Journal 876, 7 Link to Article [DOI: 10.3847/1538-4357/ab1265 ]
1Instituto de Radioastronomía y Astrofísica, UNAM, Apartado Postal 3-72, 58089 Morelia Michoacán, México
2Department of Astronomy, Boston University, 725 Commonwealth Avenue, Boston, MA 02215, USA
3Instituto de Astrofísica de Andalucía (CSIC) Glorieta de la Astronomía s/n E-18008 Granada, Spain
4Max Planck Institute fűr Astronomy (MPIA), Kőnigsthul 17, D-69117 Heidelberg, Germany

We study dust concentration in axisymmetric gas rings in protoplanetary disks. Given the gas surface density, we derived an analytical total dust surface density by taking into account the differential concentration of all grain sizes. This model allows us to predict the local dust-to-gas mass ratio and the slope of the particle size distribution, as a function of radius. We test this analytical model by comparing it with a 3D magnetohydrodynamical simulation of dust evolution in an accretion disk. The model is also applied to the disk around HD 169142. By fitting the disk continuum observations simultaneously at λ = 0.87, 1.3, and 3.0 mm, we obtain a global dust-to-gas mass ratio ${\epsilon }_{\mathrm{global}}=1.05\times {10}^{-2}$ and a viscosity coefficient α = 1.35 × 10−2. This model can be easily implemented in numerical simulations of accretion disks.

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