arXiv 1601.014492016-01-07astro-ph.SR

圆盘中CO和[ CI ]的观测和模拟。[ CI ]的首次检测和对碳丰度的限制

Observations and modelling of CO and [CI] in disks. First detections of [CI] and constraints on the carbon abundance

M. Kama, S. Bruderer, M. Carney, M. Hogerheijde, E. F. van Dishoeck, D. Fedele, A. Baryshev, W. Boland, R. Güsten, A. Aikutalp, Y. Choi, A. Endo, W. Frieswijk, … 展开作者

M. Kama, S. Bruderer, M. Carney, M. Hogerheijde, E. F. van Dishoeck, D. Fedele, A. Baryshev, W. Boland, R. Güsten, A. Aikutalp, Y. Choi, A. Endo, W. Frieswijk, A. Karska, P. Klaassen, E. Koumpia, L. Kristensen, S. Leurini, Z. Nagy, J. -P. Perez Beaupuits, C. Risacher, N. van der Marel, T. A. van Kempen, R. J. van Weeren, F. Wyrowski, U. A. Yıldız

备注：: 8 figures, accepted for publication in A\&A
发表信息：: A&A 588, A108 (2016)
DOI：: 10.1051/0004-6361/201526791

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摘要：

原行星盘中碳的气固收支与其中形成的行星的核心和大气的成分有关。关键的气相碳载体CO、C $^{0}$和C $^{+}$现在可以在圆盘中观察到。在磁盘的气相碳丰度尚未得到很好的表征，我们的目标是获得新的限制的[C]/[H]比在磁盘的样本，并得到一个概述的强度[CI]和温暖的CO排放。我们对CO $\,6$ -$5$和[CI] $\,1$ - $0$和$2$ -$1$系向具有APEX的$37$磁盘进行了调查，并用文献中的[CII]数据对其进行了补充。使用DALI代码生成的模型网格解释数据。我们还研究了如何以及气相碳丰度可以确定的参数的不确定性。在$33$来源的$13$中检测到CO $\,6$ - $5$系，在$12$来源的$6$中检测到[CI] $\,1$ - $0$，在$33$来源的$1$中检测到[CI] $\,2$ - $1$。通过深度积分，在TW~Hya和HD~100546中首次获得了盘中[CI]~ $1$-$0$的明确探测。可以基于CO和[CI]检测稳健地识别因子$5$-$10$或更多的气相碳丰度减少。TW~Hya中的原子碳检测证实了该盘中[C]/[H] $_{\rm gas}$的因子$100$还原，而数据与HD~100546的ISM样碳丰度一致。此外，BP~Tau、T~Cha、HD~139614、HD~141569和HD~100453是贫碳或贫气盘。调查中$2$ -- $1$检出率低主要反映了对T-Tauri盘的检测灵敏度不足。CO和[CII]低于模型上限的Herbig~Ae/Be盘是类碎片盘系统。与我们的调查相比，需要在灵敏度上增加大约一个数量级，以获得大多数目标系统中气相[C]/[H]比的有用约束。

英文摘要：

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 key gas-phase carbon carriers CO, C$^{0}$ and C$^{+}$ can now be observed in disks. The gas-phase carbon abundance in disks has not yet been well characterized, we aim to obtain new constraints on the [C]/[H] ratio in a sample of disks, and to get an overview of the strength of [CI] and warm CO emission. We carried out a survey of the CO$\,6$--$5$ and [CI]$\,1$--$0$ and $2$--$1$ lines towards $37$ disks with APEX, and supplemented it with [CII] data from the literature. The data are interpreted using a grid of models produced with the DALI code. We also investigate how well the gas-phase carbon abundance can be determined in light of parameter uncertainties. The CO$\,6$--$5$ line is detected in $13$ out of $33$ sources, the [CI]$\,1$--$0$ in $6$ out of $12$, and the [CI]$\,2$--$1$ in $1$ out of $33$. With deep integrations, the first unambiguous detections of [CI]~$1$--$0$ in disks are obtained, in TW~Hya and HD~100546. Gas-phase carbon abundance reductions of a factor $5$--$10$ or more can be identified robustly based on CO and [CI] detections. The atomic carbon detection in TW~Hya confirms a factor $100$ reduction of [C]/[H]$_{\rm gas}$ 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 [CI]~$2$--$1$ detection rates in the survey mostly reflect insufficient sensitivity to detect T~Tauri disks. The Herbig~Ae/Be disks with CO and [CII] upper limits below the models are debris disk like systems. A roughly order of magnitude increase in sensitivity compared to our survey is required to obtain useful constraints on the gas-phase [C]/[H] ratio in most of the targeted systems.

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