| People | Locations | Statistics |
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| Naji, M. |
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| Motta, Antonella |
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| Aletan, Dirar |
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| Mohamed, Tarek |
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| Ertürk, Emre |
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| Taccardi, Nicola |
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| Kononenko, Denys |
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| Petrov, R. H. | Madrid |
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| Alshaaer, Mazen | Brussels |
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| Bih, L. |
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| Casati, R. |
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| Muller, Hermance |
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| Kočí, Jan | Prague |
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| Šuljagić, Marija |
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| Kalteremidou, Kalliopi-Artemi | Brussels |
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| Azam, Siraj |
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| Ospanova, Alyiya |
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| Blanpain, Bart |
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| Ali, M. A. |
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| Popa, V. |
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| Rančić, M. |
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| Ollier, Nadège |
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| Azevedo, Nuno Monteiro |
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| Landes, Michael |
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| Rignanese, Gian-Marco |
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Dominik, Carsten
University of Amsterdam
in Cooperation with on an Cooperation-Score of 37%
Topics
Publications (9/9 displayed)
- 2024The polarisation properties of the HD 181327 debris ring. Evidence for sub-micron particles from scattered light observationscitations
- 2023The polarisation properties of the HD 181327 debris ring. Evidence for sub-micron particles from scattered light observations
- 2023Fractal Aggregates of Submicron-sized Grains in the Young Planet-forming Disk around IM Lupcitations
- 2022Locating dust and molecules in the inner circumstellar environment of R Sculptoris with MATISSEcitations
- 2014Rolling friction of adhesive microspherescitations
- 2014Dusty tails of evaporating exoplanets. I. Constraints on the dust compositioncitations
- 2010Dust Evolution in Protoplanetary Disks Around Herbig Ae/Be Stars—the Spitzer Viewcitations
- 2009The inner rim structures of protoplanetary discscitations
- 2006Water ice growth around evolved stars. II. Modeling infrared spectracitations
Places of action
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article
The inner rim structures of protoplanetary discs
Abstract
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 47~L<SUB>☉</SUB> 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....