H2O and OH Gas in the Terrestrial Planet-forming Zones of Protoplanetary Disks

By C. Salyk, K. Pontoppidan, G. Blake, F. Lahuis, E. V. van Dishoeck, N. Evans II. 2008

188 citations recorded by the source corpus.

We present detections of numerous 10-20 μm H2O emission lines from two protoplanetary disks around the T Tauri stars AS 205A and DR Tau, obtained using the InfraRed Spectrograph on the Spitzer Space Telescope. Follow-up 3-5 μm Keck NIRSPEC data confirm the presence of abundant water and spectrally resolve the lines. We also detect the P4.5 (2.934 μm) and P9.5 (3.179 μm) doublets of OH and 12CO/13CO v = 1 → 0 emission in both sources. Line shapes and LTE models suggest that the emission from all three molecules originates between ~0.5 and 5 AU, and so will provide a new window for understanding the chemical environment during terrestrial planet formation. LTE models also imply significant columns of H2O and OH in the inner disk atmospheres, suggesting physical transport of volatile ices either vertically or radially, while the significant radial extent of the emission stresses the importance of a more complete understanding of nonthermal excitation processes.

Subfields: Astronomy and Astrophysics, Atmospheric Science, Spectroscopy

View Paper: https://www.semanticscholar.org/paper/70c325504cc7ea5d692bfb067fc9cf63acc1e86b

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. E. Bergin
2. P. Caselli
3. Cecilia Ceccarelli
4. K. Oberg
5. Simon Bruderer
6. E. Herbst
7. E. Dishoeck
8. C. Dullemond

In Atmospheric Science

1. E. Herbst
2. P. Caselli
3. E. Bergin
4. Cecilia Ceccarelli
5. C. Walsh
6. K. Oberg
7. E. V. van Dishoeck
8. T. Millar

In Spectroscopy

1. E. Bergin
2. Cecilia Ceccarelli
3. P. Caselli
4. K. Oberg
5. C. Dullemond
6. E. Herbst
7. L. Cieza
8. C. Walsh

Citations in the corpus

• A SPITZER SURVEY OF MID-INFRARED MOLECULAR EMISSION FROM PROTOPLANETARY DISKS. I. DETECTION RATES (2010, methodology): “The lines have been shown to be excited in the 0.1-10 AU region of the disk, corresponding to the planetforming zone (Carr & Najita 2008; Salyk et al. 2008; Pontoppidan et al. 2009; Meijerink et al. 2009).”
• Protoplanetary Disks and Their Evolution (2011, result): “Salyk et al. (2008) found similar results toward an additional two disks, and the large survey by Pontoppidan et al. (2010) shows that these lines are common in T Tauri disks.”
• Complex organic molecules in protoplanetary disks (2013, methodology): “Most detections of line emission in the mid-IR have been conducted with theSpitzer Space Telescope and molecules observed include OH, H2O, C2H2, HCN, CO, and CO2 (Lahuis et al. 2006; Carr & Najita 2008; Salyk et al. 2008; Pontoppidan et al. 2010; Bast et al. 2013).”
• The Inner Regions of Protoplanetary Disks (2010, background): “…why YSO disks do not show stronger emission from molecules in the dust-free inner disk, given that the molecular emission is regularly seen in the surface layers of the disk in the dusty regions of these disks (Carr & Najita, 2008; Mandell et al., 2008; Salyk et al., 2008; Bitner et al., 2008).”
• Radiation thermo-chemical models of protoplanetary disks I. Hydrostatic disk structure and inner rim (2009, background): “More recently, near-IR gas lineshave also been detected in Spitzer IRS spectra, revealing the presence of water, H2 and the importance of X-rays (Pascucci et al., 2007; Lahuis et al., 2007; Salyk et al., 2008).”
• CHEMICAL PROCESSES IN PROTOPLANETARY DISKS (2010, background): “The molecules detected thus far at infra-red wavelengths are CO, HCN, OH, H2O, CO2 and C2H2 (Carr et al. 2004; Lahuis et al. 2006; Carr & Najita 2008; Salyk et al. 2008; Pascucci et al. 2009) with an upper limit determined for CH4 (Gibb et al. 2007).”
• 2018 Census of Interstellar, Circumstellar, Extragalactic, Protoplanetary Disk, and Exoplanetary Molecules (2018, unknown): “…[24] Öberg et al. (2015) [25] Ohashi et al. (1991) [26] Qi et al. (2003) [27] Qi et al. (2008) [28] Qi et al. (2013) [29] Salinas et al. (2016) [30] Salyk et al. (2008) [31] Sargent & Beckwith (1987) [32] Smith et al. (2009) [33] Thi et al. (1999) [34] Thi et al. (2011) [35] Walsh et al. (2016)…”
• The molecular composition of the planet-forming regions of protoplanetary disks across the luminosity regime (2015, methodology): “…or absorption, including, OH, H2O, and CH4, in several nearby disks using both Spitzer and ground-based facilities (see, e.g., Carr & Najita 2008; Salyk et al. 2008; Pascucci et al. 2009; Pontoppidan et al. 2010; Carr & Najita 2011; Fedele et al. 2011; Salyk et al. 2011; Mandell et al. 2012;…”
• Spectroastrometric Imaging of Molecular Gas within Protoplanetary Disk Gaps (2008, background): “Spatially resolving the emission from other molecules, in particular the water lines recently reported in Salyk et al. (2008), is likely within the capability of CRIRES, and would directly probe the chemical variations in the planetforming region of circumstellar disks.”
• Our astrochemical heritage (2012, background): “[311]; [277]; [414]; [184]), H2 ([36]; [156]), as well as near-infrared lines of CO, H2O, OH ([386]; [77]; [358]) and simple organic molecules ([278]).”
• Astrochemistry and compositions of planetary systems (2020, background): “2019a), but HCN is also observed at IR wavelengths, and C2H2 is only observed at these shorter wavelengths due to its lack of a permanent dipole moment (Carr and Najita 2008; Salyk et al. 2008; Najita et al. 2010).”