Hostname: page-component-7bb8b95d7b-dtkg6 Total loading time: 0 Render date: 2024-10-06T08:10:22.328Z Has data issue: false hasContentIssue false
  • English
  • Français

Cosmic Rays and the Origin of Volatiles in Protoplanetary Disks

Published online by Cambridge University Press:  27 January 2016

Germán Chaparro-Molano  and
Inga Kamp
Germán Chaparro-Molano
Affiliation:
Universidad ECCI, Bogotá, Colombia email: [email protected]
Inga Kamp
Affiliation:
Kapteyn Astronomical Institute, Rijksuniversiteit Groningen, The Netherlands email: [email protected]
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The origin of water and other volatiles in protoplanetary disks can be either interstellar or due to chemical processing during the protoplanetary disk phase. Depending on the strength of the ionization field present during this stage, an active chemical evolution in the protoplanetary disk midplane can lead to formation of complex volatiles on timescales shorter than the disk dissipation timescale. For this reason, we investigate the effects of cosmic rays and the usually neglected cosmic ray induced UV ionization field in time dependent chemical models of protoplanetary disks. These results are benchmarked against our current knowledge of the chemical composition of cometary ices. We conclude that water and other, more complex volatiles can be preserved in the ice mantles of dust grains. This ice mantle growth can also have a significant impact on the dust opacity and hence on the temperature profile of the disk midplane. This effect will be observable in the near future with ALMA.

Keywords

AstrochemistryComets: GeneralProtoplanetary Disks(ISM:) Cosmic Rays
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 10 , Issue S314: Young Stars & Planets Near the Sun , November 2015 , pp. 189 - 190
Copyright
Copyright © International Astronomical Union 2016 

References

Acharyya, K., Hassel, G. E., & Herbst, E. 2011, ApJ, 732, 73CrossRefGoogle Scholar
Bockelee-Morvan, D. 2010, in Physics and Astrophysics of Planetary Systems, EAS Publication Series, 41, 313Google Scholar
Chaparro Molano, G. & Kamp, I. 2012, A&A, 537, A138Google Scholar
Chang, Q., Cuppen, H. M., & Herbst, E. 2007, A&A, 469, 973Google Scholar
Ferrín, I. 2013, MNRAS 442 2, p.1731Google Scholar
Tielens, A. G. G. M. & Hagen, W. 1982, A&A, 114, 245Google Scholar
Visser, R., van Dishoeck, E. F., Doty, S. D., & Dullemond, C. P. 2009, A&A, 495, 881Google Scholar
Woitke, P., Kamp, I., & Thi, W.-F. 2009, A&A, 501, 383Google Scholar
Woodall, J., Agúndez, M., Markwick-Kemper, A. J., & Millar, T. J. 2007, A&A, 466, 1197Google Scholar