F. Meru, M. Galvagni, C. Olczak, and P. Garaud. (2013)cite arxiv:1308.5181Comment: Submitted to the conference proceedings of the IAU Symposium 299 - Exploring the formation and evolution of planetary systems. 2 pages; 2 figures.
We perform coagulation & fragmentation simulations to understand grain growth
in T Tauri & brown dwarf discs. We present a physically-motivated approach
using a probability distribution function for the collision velocities and
separating the deterministic & stochastic velocities. We find growth to larger
sizes compared to other models. Furthermore, if brown dwarf discs are
scaled-down versions of T Tauri discs (in terms of stellar & disc mass, and
disc radius), growth at the same location with respect to the outer edge occurs
to similar sizes in both discs.(more)
cite arxiv:1308.5181Comment: Submitted to the conference proceedings of the IAU Symposium 299 - Exploring the formation and evolution of planetary systems. 2 pages; 2 figures
Please log in to take part in the discussion (add own reviews or comments).
Cite this publication
More citation styles
- please select -
%0 Generic
%1 meru2013large
%A Meru, Farzana
%A Galvagni, Marina
%A Olczak, Christoph
%A Garaud, Pascale
%D 2013
%K 2013 PPD coagulation formation planets
%T Large grains can grow in circumstellar discs
%U http://arxiv.org/abs/1308.5181
%X We perform coagulation & fragmentation simulations to understand grain growth
in T Tauri & brown dwarf discs. We present a physically-motivated approach
using a probability distribution function for the collision velocities and
separating the deterministic & stochastic velocities. We find growth to larger
sizes compared to other models. Furthermore, if brown dwarf discs are
scaled-down versions of T Tauri discs (in terms of stellar & disc mass, and
disc radius), growth at the same location with respect to the outer edge occurs
to similar sizes in both discs.
@misc{meru2013large,
abstract = {We perform coagulation & fragmentation simulations to understand grain growth
in T Tauri & brown dwarf discs. We present a physically-motivated approach
using a probability distribution function for the collision velocities and
separating the deterministic & stochastic velocities. We find growth to larger
sizes compared to other models. Furthermore, if brown dwarf discs are
scaled-down versions of T Tauri discs (in terms of stellar & disc mass, and
disc radius), growth at the same location with respect to the outer edge occurs
to similar sizes in both discs.},
added-at = {2013-08-26T09:51:59.000+0200},
author = {Meru, Farzana and Galvagni, Marina and Olczak, Christoph and Garaud, Pascale},
biburl = {https://www.bibsonomy.org/bibtex/2f6fd59b369824c625e8fab5e719afc3b/danielcarrera},
description = {[1308.5181] Large grains can grow in circumstellar discs},
interhash = {7cccab11f6e86e8a42869f32b8a73859},
intrahash = {f6fd59b369824c625e8fab5e719afc3b},
keywords = {2013 PPD coagulation formation planets},
note = {cite arxiv:1308.5181Comment: Submitted to the conference proceedings of the IAU Symposium 299 - Exploring the formation and evolution of planetary systems. 2 pages; 2 figures},
timestamp = {2014-07-25T17:15:44.000+0200},
title = {Large grains can grow in circumstellar discs},
url = {http://arxiv.org/abs/1308.5181},
year = 2013
}