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Gas evolution in protoplanetary disks

Published online by Cambridge University Press:  26 May 2016

W. F. Thi ,
E.F. van Dishoeck ,
G.J. van Zadelhoff ,
G. A. Blake ,
V. Mannings ,
A. I. Sargent ,
J. Horn ,
E. E. Becklin ,
M.E. van den Ancker  and
A. Natta
W. F. Thi
Affiliation:
Leiden Observatory, P.O. Box 9513, 2300 Leiden, The Netherlands
E.F. van Dishoeck
Affiliation:
Leiden Observatory, P.O. Box 9513, 2300 Leiden, The Netherlands
G.J. van Zadelhoff
Affiliation:
Leiden Observatory, P.O. Box 9513, 2300 Leiden, The Netherlands
G. A. Blake
Affiliation:
California Institute of Technology, Pasadena, CA, USA
V. Mannings
Affiliation:
California Institute of Technology, Pasadena, CA, USA
A. I. Sargent
Affiliation:
California Institute of Technology, Pasadena, CA, USA
J. Horn
Affiliation:
UCLA, Los Angeles, CA, USA
E. E. Becklin
Affiliation:
UCLA, Los Angeles, CA, USA
M.E. van den Ancker
Affiliation:
Harvard–Smithsonian Center for Astrophysics, Cambridge, MA, USA
A. Natta
Affiliation:
Osservatorio Astrofisico di Arcetri, Firenze, Italy

Abstract

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We present the results of a study of the evolution of the gas and dust in disks around T Tauri, Herbig Ae and Vega-like stars. We observed the two lowest rotational lines of H2 with the ISO-SWS as well as 12CO 3–2 and 13CO 3–2 with the JCMT, and CO 6–5 with the CSO. The H2 lines trace the warm (∽ 100 K) inner region whereas the CO lines probe the colder outer disks. Substantial amounts of H2 have been detected toward T Tauri and Herbig Ae stars, and, surprisingly, also around three Vega-like objects (49 Cet, HD 135344 and β Pictoris). In contrast with previous conclusions derived from CO data, a significant mass of warm gas is found to persist up to ages of several tens of Myrs, suggesting that slow formation of gas-rich giant planets is possible.

Type
Part IV: Protoplanetary and β Pic disks
Information
Symposium - International Astronomical Union , Volume 202: Planetary Systems in the Universe – Observation, Formation and Evolution , 2004 , pp. 378 - 380
Copyright
Copyright © Astronomical Society of the Pacific 2004 

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