Instruct: Identify the main and secondary category of Arxiv papers based on the titles and abstracts
Query: Influence of grain growth on the thermal structure of protoplanetary
  discs   The thermal structure of a protoplanetary disc is regulated by the opacity
that dust grains provide. However, previous works have often considered
simplified prescriptions for the dust opacity in hydrodynamical disc
simulations, e.g. by considering only a single particle size. In the present
work we perform 2D hydrodynamical simulations of protoplanetary discs where the
opacity is self-consistently calculated for the dust population, taking into
account the particle size, composition and abundance. We first compare
simulations using single grain sizes to two different multi-grain size
distributions at different levels of turbulence strengths, parameterized
through the $\alpha$-viscosity, and different gas surface densities. Assuming a
single dust size leads to inaccurate calculations of the thermal structure of
discs, because the grain size dominating the opacity increases with orbital
radius. Overall the two grain size distributions, one limited by fragmentation
only and the other determined from a more complete fragmentation-coagulation
equilibrium, give similar results for the thermal structure. We find that both
grain size distributions give less steep opacity gradients that result in less
steep aspect ratio gradients, in comparison to discs with only micrometer sized
dust. Moreover, in the discs with a grain size distribution, the innermost
outward migration region is removed and planets embedded is such discs
experience lower migration rates. We also investigate the dependency of the
water iceline position on the alpha-viscosity, the initial gas surface density
at 1 AU and the dust-to-gas ratio and find $r_{ice} \propto \alpha^{0.61}
\Sigma_{g,0}^{0.8} f_{DG}^{0.37}$ independently of the distribution used. The
inclusion of the feedback loop between grain growth, opacities and disc
thermodynamics allows for more self-consistent simulations of accretion discs
and planet formation.

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The categories of this paper are: stat
28
The categories of this paper are: alg-geom
30
The categories of this paper are: q-alg
14
The categories of this paper are: math-ph
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The categories of this paper are: q-bio
34
The categories of this paper are: chem-ph
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The categories of this paper are: eess
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The categories of this paper are: q-fin
9
The categories of this paper are: nlin
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The categories of this paper are: chao-dyn
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The categories of this paper are: hep-lat
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The categories of this paper are: econ
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The categories of this paper are: acc-phys
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The categories of this paper are: funct-an
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The categories of this paper are: cs
31
The categories of this paper are: ao-sci