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Rings, rings, rings: what does CN tell us?

Published online by Cambridge University Press:  04 September 2018

Paolo Cazzoletti Open the ORCID record for Paolo Cazzoletti [Opens in a new window]
Paolo Cazzoletti*
Affiliation:
Max-Planck-Institut für Extraterrestrische Physik, Gieenbachstrae, 85741, Garching bei München, Germany email: pcazzoletti@mpe.mpg.de
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Abstract

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CN emission lines are among the brightest, and have been observed in the last 20 years with single dish observations. With modern interferometers, we are now able to spatially resolve CN emission, which often shows ring-like structures. We investigate whether such structures trace the morphology of the disks, or if they have a chemical origin. By using the thermochemical code DALI, we conclude that CN formation is triggered by the existence of vibrationally excited H2*, produced by FUV pumping of H2. Herbig stars therefore generally have larger rings and higher CN fluxes than TTauri. Disks with higher masses and flaring also show stronger CN emission and larger rings. CN observations could in the future provide important constraints on some important disk physical parameters. The results of the models are well consistent with the spatially resolved CN observations to-date available.

Keywords

astrochemistryplanetary systems: protoplanetary disks –methods: numerical – radiative transfer
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 13 , Symposium S332: Astrochemistry VII: Through the Cosmos from Galaxies to Planets , March 2017 , pp. 233 - 236
Copyright
Copyright © International Astronomical Union 2018 

References

Bruderer, S., 2013, A&A, 559, A46Google Scholar
Cazzoletti, P., van Dishoeck, E. F., Visser, R., Facchini, F., & Bruderer, S. in press on A&AGoogle Scholar
Chapillon, E., Guilloteau, S., Dutrey, A., Piétu, V., & Guélin, M., 2012, A&A, 537, A60Google Scholar
Dutrey, A., Guilloteau, S., & Guelin, M., 1997, A&A, 317, L55Google Scholar
Guilloteau, S., Simon, M., Piétu, V., et al. 2014, A&A, 567, A117Google Scholar
Guilloteau, S., Reboussin, L., Dutrey, A., et al. 2016, A&A, 592, A124Google Scholar
Kastner, J. H., Zuckerman, B., Hily-Blant, P., & Forveille, T., 2008, A&A, 492, 469Google Scholar
Kastner, J. H., Hily-Blant, P., Rodriguez, D. R., Punzi, K., & Forveille, T., 2014, ApJ, 793, 55Google Scholar
Öberg, K. I., Qi, C., Fogel, J. K. J., et al. 2010, ApJ, 720, 480Google Scholar
Öberg, K. I., Qi, C., Fogel, J. K. J., et al. 2011, ApJ, 734, 98Google Scholar
Salter, D. M., Hogerheijde, M. R., van der Burg, R. F. J., Kristensen, L. E., & Brinch, C., 2011, A&A, 536, A80Google Scholar
Teague, R., Guilloteau, S., Semenov, D., et al. 2016, A&A, 592, A49Google Scholar
Thi, W.-F., van Zadelhoff, G.-J., & van Dishoeck, E. F., 2004, A&A, 425, 955Google Scholar
van Terwisga, S., van Dishoeck, E. F., Facchini, F., Cazzoletti, P., et al. in prep.Google Scholar
Visser, R., Bruderer, S., Cazzoletti, P., Facchini, S., Heays, A. and van Dishoeck, E. F. in prep.Google Scholar