Volume 506, Number 3, November II 2009
|Page(s)||1199 - 1213|
|Section||Interstellar and circumstellar matter|
|Published online||18 August 2009|
The inner rim structures of protoplanetary discs
Anton Pannekoek Astronomical Institute, University of Amsterdam, PO Box 94249, 1090 GE Amsterdam, The Netherlands e-mail: M.Kama@uva.nl
2 Utrecht Astronomical Institute, University of Utrecht, PO Box 80000, 3508 TA Utrecht, The Netherlands
3 Department of Astrophysics, Radboud University Nijmegen, Postbus 9010, 6500 GL Nijmegen, The Netherlands
Accepted: 27 July 2009
The inner boundary of protoplanetary discs is structured by the dramatic opacity changes at the transition from the dust-containing to a dust-free zone. This paper explores the variety and limits of inner rim structures in passively heated dusty discs. For this study, we implemented detailed sublimation physics in a fast Monte Carlo radiative transfer code. We show that the inner rim in dusty discs is not an infinitely sharp wall but a diffuse region which may be narrow or wide. Furthermore, high surface densities and large silicate grains as well as iron and corundum grains decrease the rim radius, from a 2.2 AU radius for small silicates around a Herbig Ae star typically to 0.4 AU and as close as 0.2 AU. A passive disc with grain growth and a diverse dust composition must thus have a small inner rim radius. Finally, an analytical expression is presented for the rim location as a function of dust, disc and stellar properties.
Key words: stars: circumstellar matter / stars: planetary systems: protoplanetary disks
© ESO, 2009
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.