Volatile carbon locking and release in protoplanetary disks. A study of TW Hya and HD 100546
By M. Kama, Simon Bruderer, E. Dishoeck, M. Hogerheijde, C. Folsom, A. Miotello, D. Fedele, Arnaud Belloche, R. Güsten, F. Wyrowski. 2016
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The composition of planetary solids and gases is largely rooted in the processing of volatile elements in protoplanetary disks. To shed light on the key processes, we carry out a comparative analysis of the gas-phase carbon abundance in two systems with a similar age and disk mass, but different central stars: HD 100546 and TW Hya. We combine our recent detections of C$^{0}$ in these disks with observations of other carbon reservoirs (CO, C$^{+}$, C$_{2}$H) and gas mass and warm gas tracers (HD, O$^{0}$), as well as spatially resolved ALMA observations and the spectral energy distribution. The disks are modelled with the DALI 2D physical-chemical code. Stellar abundances for HD 100546 are derived from archival spectra. Upper limits on HD emission from HD 100546 place an upper limit on the total disk mass of $\leq0.1\,M_{\odot}$. The gas-phase carbon abundance in the atmosphere of this warm Herbig disk is at most moderately depleted compared to the interstellar medium, with [C]/[H]$_{\rm gas}=(0.1-1.5)\times 10^{-4}$. HD 100546 itself is a $\lambda\,$Bootis star, with solar abundances of C and O but a strong depletion of rock-forming elements. In the gas of the T Tauri disk TW Hya, both C and O are strongly underabundant, with [C]/[H]$_{\rm gas}=(0.2-5.0)\times 10^{-6}$ and C/O${>}1$. We discuss evidence that the gas-phase C and O abundances are high in the warm inner regions of both disks. Our analytical model, including vertical mixing and a grain size distribution, reproduces the observed [C]/[H]$_{\rm gas}$ in the outer disk of TW Hya and allows to make predictions for other systems.
Subfields: Astronomy and Astrophysics, Spectroscopy
View Paper: https://www.semanticscholar.org/paper/9035b4bc8d66c29b901c392d49df9aac67de740d
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Citations in the corpus
- A Three-dimensional View of Turbulence: Constraints on Turbulent Motions in the HD 163296 Protoplanetary Disk Using DCO+ (2017, background): “Recent work has brought into question standard assumptions about the gas-to-dust mass ratio, CO/H2, and C18O/CO (Bergin et al. 2013; Miotello et al. 2014; Ansdell et al. 2016; Kama et al. 2016), raising the possibility of a significant deviation from our assumed disk mass.”
- Turbulence in the TW Hya Disk (2018, methodology): “Synthetic CO data are generated based on the temperature, density, and abundance distribution from Kama et al. (2016), and fed through LIME (Brinch & Hogerheijde 2010) to generate model images of CO(2-1).”
- Astrochemistry and compositions of planetary systems (2020, background): “Some patterns that are emerging is that it is difficult to explain the relative abundances of nitrogen and oxygen bearing organics unless the disk atmospheres are C-rich and/or O-poor (Bergin et al. 2016; Kama et al. 2016; Cleeves et al. 2018; Le Gal et al. 2019b), that O-bearing organics are presen”