Volume 600, April 2017
|Number of page(s)||16|
|Section||Interstellar and circumstellar matter|
|Published online||14 April 2017|
Redistribution of CO at the location of the CO ice line in evolving gas and dust disks
1 Heidelberg University, Center for Astronomy, Institute of Theoretical Astrophysics, Albert-Ueberle-Straße 2, 69120 Heidelberg, Germany
2 Instituto de Astrofísica, Facultad de Física, Pontificia Universidad Católica de Chile, Santiago, Chile
3 Max Planck Institute for Astronomy, Königstuhl 17, 69117 Heidelberg, Germany
4 Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
5 School of Physics and Astronomy, The University of Leeds, E. C. Stoner Building, Leeds LS2 9JT, UK
6 Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge, CB3 0HA, UK
7 University of Amsterdam, Astronomical Institute Anton Pannekoek, Postbus 94249, 1090 GE Amsterdam, The Netherlands
Received: 2 June 2016
Accepted: 5 January 2017
Context. Ice lines are suggested to play a significant role in grain growth and planetesimal formation in protoplanetary disks. Evaporation fronts directly influence the gas and ice abundances of volatile species in the disk and therefore the coagulation physics and efficiency and the chemical composition of the resulting planetesimals.
Aims. In this work, we investigate the influence of the existence of the CO ice line on particle growth and on the distribution of CO in the disk.
Methods. We include the possibility of tracking the CO content and/or other volatiles in particles and in the gas in our existing dust coagulation and disk evolution model and present a method for studying evaporation and condensation of CO using the Hertz-Knudsen equation. Our model does not yet include fragmentation, which will be part of further investigations.
Results. We find no enhanced grain growth immediately outside the ice line where the particle size is limited by radial drift. Instead, we find a depletion of solid material inside the ice line, which is solely due to evaporation of the CO. Such a depression inside the ice line may be observable and may help to quantify the processes described in this work. Furthermore, we find that the viscosity and diffusivity of the gas heavily influence the re-distribution of vaporized CO at the ice line and can lead to an increase in the CO abundance by up to a factor of a few in the region just inside the ice line. Depending on the strength of the gaseous transport mechanisms, the position of the ice line in our model can change by up to ~ 10 AU and consequently, the temperature at that location can range from 21 to 23 K.
Key words: protoplanetary disks / accretion, accretion disks / diffusion / methods: numerical
© ESO, 2017
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