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Chasing disk dispersal indicators: the origin of the [OI] low-velocity components from young stars

Published online by Cambridge University Press:  06 January 2014

Elisabetta Rigliaco ,
Ilaria Pascucci ,
Uma Gorti ,
Suzan Edwards  and
David Holenbach
Elisabetta Rigliaco
Affiliation:
Lunar and Planetary Laboratory, The University of Arizona, Tucson, AZ 85721, USAs email: rigliaco@lpl.arizona.edu
Ilaria Pascucci
Affiliation:
Lunar and Planetary Laboratory, The University of Arizona, Tucson, AZ 85721, USAs email: rigliaco@lpl.arizona.edu
Uma Gorti
Affiliation:
SETI Institute, Mountain View, CA, USA NASA Ames Research Center, Moffett Feld, CA
Suzan Edwards
Affiliation:
Astronomy Department, Smith College, Northampton, MA 01063
David Holenbach
Affiliation:
SETI Institute, Mountain View, CA, USA
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Abstract

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Understanding how a disk surrounding a young star evolves and disperses is crucial in order to understand the subsequent planet formation. In this proceeding, we summarize the results reported by Rigliaco et al. (2013) on the origin of the [OI] low-velocity component as a possible disk dispersal indicator.

Keywords

accretionaccretion disks – stars: formation – planetary systems:protoplanetary disks – stars: pre–main-sequence – ultraviolet:stars
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S299: Exploring the Formation and Evolution of Planetary Systems , June 2013 , pp. 226 - 227
Copyright
Copyright © International Astronomical Union 2013 

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