Modelling accretion in transitional disks
| Autor: | Tobias W. A. Müller, Wilhelm Kley |
|---|---|
| Rok vydání: | 2013 |
| Předmět: |
Earth and Planetary Astrophysics (astro-ph.EP)
Physics Mass flow FOS: Physical sciences Astronomy and Astrophysics Astrophysics Protoplanetary disk Accretion (astrophysics) Space and Planetary Science Planet Mass flow rate Radiative transfer Astrophysics::Earth and Planetary Astrophysics Low Mass Planetary mass Astrophysics::Galaxy Astrophysics Astrophysics - Earth and Planetary Astrophysics |
| Zdroj: | Astronomy & Astrophysics. 560:A40 |
| ISSN: | 1432-0746 0004-6361 |
| DOI: | 10.1051/0004-6361/201322503 |
| Popis: | Transitional disks are protoplanetary disk around young stars that display inner holes in the dust distribution within a few AU, which is accompanied nevertheless by some gas accretion onto the central star. These cavities could possibly be created by the presence of one or more massive planets. If the gap is created by planets and gas is still present in it, then there should be a flow of gas past the planet into the inner region. It is our goal to study the mass accretion rate into the gap and in particular the dependency on the planet's mass and the thermodynamic properties of the disk. We performed 2D hydro simulations for disks with embedded planets. We added radiative cooling from the disk surfaces, radiative diffusion in the disk midplane, and stellar irradiation to the energy equation to have more realistic models. The mass flow rate into the gap region depends, for given disk thermodynamics, non-monotonically on the mass of the planet. Generally, more massive planets open wider and deeper gaps which would tend to reduce the mass accretion into the inner cavity. However, for larger mass planets the outer disk becomes eccentric and the mass flow rate is enhanced over the low mass cases. As a result, for the isothermal disks the mass flow is always comparable to the expected mass flow of unperturbed disks M_d, while for more realistic radiative disks the mass flow is very small for low mass planets ( 10 pages, 29 figures, accepted for publication in Astronomy & Astrophysics |
| Databáze: | OpenAIRE |
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