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Issue A&A
Volume 453, Number 1, July I 2006
Page(s) 163 - 171
Section Interstellar and circumstellar matter
DOI http://dx.doi.org/10.1051/0004-6361:20054769



A&A 453, 163-171 (2006)
DOI: 10.1051/0004-6361:20054769

Modeling the gas-phase chemistry of the transitional disk around HD 141569A

B. Jonkheid1, I. Kamp2, J.-C. Augereau1, 3 and E. F. van Dishoeck1

1  Sterrewacht Leiden, PO Box 9513, 2300 RA Leiden, The Netherlands
    e-mail: jonkheid@strw.leidenuniv.nl
2  Space Telescope Division of ESA, Space Telescope Science Institute, 3700 San Martin drive, Baltimore, MD 21218, USA
3  Laboratoire d'Astrophysique, Observatoire de Grenoble, BP 53, 380431 Grenoble Cedex 9, France

(Received 23 December 2005 / Accepted 14 March 2006 )

Abstract
Aims.The chemistry, distribution and mass of the gas in the transitional disk around the 5 Myr old B9.5 V star HD 141569A are constrained.
Methods.A quasi 2-dimensional (2D) chemistry code for photon dominated regions (PDR) is used to calculate the chemistry and gas temperatures in the disk. The calculations are performed for several gas distributions, PAH abundances and values of the total gas mass. The resulting CO J=2-1 and J=3-2 emission lines are computed with a 2D radiative transfer code and are compared to observations.
Results.The CO abundance is very sensitive to the total disk mass because the disk is in a regime where self-shielding just sets in. The observed CO emission lines are best fit by a power-law gas distribution of  $80~M_\oplus$ starting at 80 AU from the central star, indicating that there is some gas in the inner hole. Predictions are made for intensities of atomic fine-structure lines. [ $\ion{C}{i}$], which is the dominant form of carbon in large parts of the disk, is found to be a good alternative tracer of the gas mass.


Key words: astrochemistry -- stars: individual: HD 141569A -- stars: planetary systems: protoplanetary disks



© ESO 2006


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