Water in protoplanetary disks

H. Nomura, C. Walsh, D. Heinzeller, T. J. Millar

Research output: Chapter in Book/Report/Conference proceedingConference contribution

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.

Original languageEnglish
Title of host publicationProceedings of the International Astronomical Union: formation, detection, and characterization of extrasolar habitable planets
PublisherCambridge University Press
Pages235-237
Number of pages3
Volume3
EditionS293
DOIs
Publication statusPublished - 29 Apr 2014

Keywords

  • line: formation
  • molecular processes
  • planetary systems: protoplanetary disks

ASJC Scopus subject areas

  • Astronomy and Astrophysics

Fingerprint Dive into the research topics of 'Water in protoplanetary disks'. Together they form a unique fingerprint.

  • Cite this

    Nomura, H., Walsh, C., Heinzeller, D., & Millar, T. J. (2014). Water in protoplanetary disks. In Proceedings of the International Astronomical Union: formation, detection, and characterization of extrasolar habitable planets (S293 ed., Vol. 3, pp. 235-237). Cambridge University Press. https://doi.org/10.1017/S1743921313012891