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Water in Protoplanetary Disks

  • H. Nomura (a1), C. Walsh (a2), D. Heinzeller (a3) and T. J. Millar (a2)

Abstract

Infrared water line emission from protoplanetary disks, recently observed by the Spitzer and Herschel space telescopes, is thought to trace the surface layer of the inner to outer regions of the disks. We have modelled the water abundance profile and line emission, especially focusing on the effects of dust size growth and turbulent mixing. Comparison between model calculations and observations suggests a small grain model with turbulent mixing is preferred.

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References

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Cazaux, S. & Tielens, A. G. G. M. 2004, ApJ, 604, 222
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Keywords

Water in Protoplanetary Disks

  • H. Nomura (a1), C. Walsh (a2), D. Heinzeller (a3) and T. J. Millar (a2)

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