Observations and modelling of CO and [C i] in protoplanetary disks
| Autor: | Z. Nagy, A. Aikutalp, J. P. Perez Beaupuits, Akira Endo, E. F. van Dishoeck, R. Güsten, Christophe Risacher, E. Koumpia, N. van der Marel, P. D. Klaassen, Agata Karska, M. Kama, Andrey M. Baryshev, Umut A. Yildiz, Davide Fedele, Friedrich Wyrowski, Lars E. Kristensen, R. J. van Weeren, S. Leurini, W. Boland, Michiel R. Hogerheijde, T. A. van Kempen, Yun-Young Choi, M. T. Carney, S. Bruderer, W. Frieswijk |
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| Přispěvatelé: | Astronomy |
| Rok vydání: | 2016 |
| Předmět: |
Physics
Debris disk 010504 meteorology & atmospheric sciences Abundance (chemistry) protoplanetary disks chemistry.chemical_element submillimeter: planetary systems Astronomy and Astrophysics Astrophysics 01 natural sciences chemistry.chemical_compound surveys chemistry 13. Climate action Space and Planetary Science 0103 physical sciences Atomic carbon Detection rate 010303 astronomy & astrophysics Carbon Order of magnitude 0105 earth and related environmental sciences Line (formation) |
| Zdroj: | Astronomy and Astrophysics, 588, A108 Astronomy and astrophysics, 588:A108. EDP Sciences |
| ISSN: | 1432-0746 0004-6361 |
| DOI: | 10.1051/0004-6361/201526791 |
| Popis: | Context. The gas-solid budget of carbon in protoplanetary disks is related to the composition of the cores and atmospheres of the planets forming in them. The principal gas-phase carbon carriers CO, C0, and C+ can now be observed regularly in disks. Aims: The gas-phase carbon abundance in disks has thus far not been well characterized observationally. We obtain new constraints on the [C]/[H] ratio in a large sample of disks, and compile an overview of the strength of [C I] and warm CO emission. Methods: We carried out a survey of the CO 6-5 line and the [C I] 1-0 and 2-1 lines towards 37 disks with the APEX telescope, and supplemented it with [C II] data from the literature. The data are interpreted using a grid of models produced with the DALI disk code. We also investigate how well the gas-phase carbon abundance can be determined in light of parameter uncertainties. Results: The CO 6-5 line is detected in 13 out of 33 sources, [C I] 1-0 in 6 out of 12, and [C I] 2-1 in 1 out of 33. With separate deep integrations, the first unambiguous detections of the [C I] 1-0 line in disks are obtained, in TW Hya and HD 100546. Conclusions: Gas-phase carbon abundance reductions of a factor of 5-10 or more can be identified robustly based on CO and [C I] detections, assuming reasonable constraints on other parameters. The atomic carbon detection towards TW Hya confirms a factor of 100 reduction of [C]/[H]gas in that disk, while the data are consistent with an ISM-like carbon abundance for HD 100546. In addition, BP Tau, T Cha, HD 139614, HD 141569, and HD 100453 are either carbon-depleted or gas-poor disks. The low [C I] 2-1 detection rates in the survey mostly reflect insufficient sensitivity for T Tauri disks. The Herbig Ae/Be disks with CO and [C II] upper limits below the models are debris-disk-like systems. An increase in sensitivity of roughly order of magnitude compared to our survey is required to obtain useful constraints on the gas-phase [C]/[H] ratio in most of the targeted systems. The reduced spectra (FITS files) are only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/588/A108 |
| Databáze: | OpenAIRE |
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