Water in the terrestrial planet-forming zone of the PDS 70 disk

Perotti, G.; Christiaens, V.; Henning, Thomas; Tabone, B.; Waters, L. B. F. M.; Kamp, I.; Olofsson, G.; Grant, Sierra L.; Gasman, Danny; Bouwman, J.; Samland, M.; Franceschi, Riccardo; Dishoeck, Ewine van; Schwarz, Kamber R.; Güdel, M.; Lagage, P. O.; Ray, T. P.; Vandenbussche, B.; Abergel, A.; Absil, Olivier; Arabhavi, Aditya M.; Argyriou, Ioannis; Barrado, D.; Boccaletti, A.; Garatti, A. Caratti o; Geers, V. C.; Glauser, Adrian M.; Justtanont, K.; Lahuis, F.; Mueller, Michael; Nehmé, Cyrine; Pantin, E.; Scheithauer, S.; Waelkens, C.; Guadarrama, R.; Jang, Hyerin; Kanwar, J. S.; Morales-Calderón, M.; Pawellek, N.; Rodgers-Lee, D.; Schreiber, J.; Colina, L.; Greve, T. R.; Östlin, Göran; Wright, Gillian

doi:10.1038/s41586-023-06317-9

Cited by 16 publications

(14 citation statements)

References 55 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…No further forbidden emission lines, such as [S II] or [N II] were detected in the photospheric removed HARPS spectra, neither was the [O I] 5577 Å. We also note that there is no trace of [Ne II], as shown in Perotti et al (2023).…”

Section: Wind-tracing Emission Linessupporting

confidence: 49%

A Magnetically Driven Disk Wind in the Inner Disk of PDS 70*

Campbell-White,

Manara,

Benisty

et al. 2023

ApJ

View full text Add to dashboard Cite

PDS 70 is so far the only young disk where multiple planets have been detected by direct imaging. The disk has a large cavity when seen at submillimeter and near-infrared wavelengths, which hosts two massive planets. This makes PDS 70 the ideal target to study the physical conditions in a strongly depleted inner disk shaped by two giant planets, and in particular to test whether disk winds can play a significant role in its evolution. Using X-Shooter and HARPS spectra, we detected for the first time the wind-tracing [O i] 6300 Å line, and confirm the low-moderate value of mass-accretion rate in the literature. The [O i] line luminosity is high with respect to the accretion luminosity when compared to a large sample of disks with cavities in nearby star-forming regions. The FWHM and blueshifted peak of the [O i] line suggest an emission in a region very close to the star, favoring a magnetically driven wind as the origin. We also detect wind emission and high variability in the He i 10830 Å line, which is unusual for low accretors. We discuss that, although the cavity of PDS 70 was clearly carved out by the giant planets, the substantial inner-disk wind could also have had a significant contribution to clearing the inner disk.

show abstract

Section: Wind-tracing Emission Linessupporting

confidence: 49%

A Magnetically Driven Disk Wind in the Inner Disk of PDS 70*

Campbell-White,

Manara,

Benisty

et al. 2023

ApJ

View full text Add to dashboard Cite

show abstract

“…For the cooler H 2 O component the temperature is better constrained to values between ∼450 and ∼700 K. It has been pointed out in the literature that the shorter wavelengths probe H 2 O at higher temperatures, while the longer wavelengths probe the colder regions (Blevins et al 2016;Banzatti et al 2023;Gasman et al 2023). For XUE 1, although the best-fitting values agree with this behavior, when taking into account the confidence intervals, the temperature cascade does not seem to be as extreme, similarly to the case in PDS 70 (Perotti et al 2023).…”

Section: H 2 Omentioning

confidence: 57%

“…We compare our measurements with Spitzer and newly obtained JWST observations of PPDs that are not strongly irradiated, i.e., in low-mass star-forming regions. Figure 4 shows the line luminosity of H 2 O, measured from the 17 μm lines, against the HCN/H 2 O, C 2 H 2 /H 2 O, CO/H 2 O, and 12 CO 2 /H 2 O of XUE 1 in comparison with a sample of T Tauri stars located in nearby (<200 pc), young (1-3 Myr) starforming regions from Banzatti et al (2020Banzatti et al ( , 2022 and the newly obtained JWST observations of isolated PPDs (Grant et al 2023;Kóspál et al 2023;Perotti et al 2023). We find that the H 2 O luminosity and the 12 CO 2 /H 2 O ratio are at the high end of the distribution.…”

Section: Comparison To Ppds In Low-mass Star-forming Regionsmentioning

confidence: 99%

“…Since the line luminosities of XUE 1 are in the range of those observed in nonirradiated disks (see Appendix E; but note the high C 2 H 2 and HCN line luminosities; see below), disk irradiation is not needed to explain our observations. Perotti et al (2023) compare the H 2 O luminosity of a sample of disks from Banzatti et al (2020Banzatti et al ( , 2022 to the continuum spectral index n 13-30 , which is a measure of the dust depletion of the inner disk. We follow this approach, but we calculate the n 13-25 from the Spitzer spectra from the Spexodisks database (Pontoppidan et al 2010;Salyk et al 2011;Banzatti et al 2020) to allow direct comparison to our MIRI data.…”

Section: Comparison To Ppds In Low-mass Star-forming Regionsmentioning

confidence: 99%

“…The resulting velocity can then be used to provide additional constraints on the emitting surface radius provided that we know the mass of the central star, allowing us to circumvent the degeneracy between the column density and the emitting surface radius. In order to characterize the remaining molecular emission features present in the spectrum of XUE 1, we model them with the LTE model presented in Tabone et al (2023), which has also been used in Grant et al (2023), Perotti et al (2023), and Gasman et al (2023. We included emission from H 2 O (around 7 and 15 μm), 12 CO 2 , 13 CO 2 , OH, C 2 H 2 , and HCN, with molecular data from the HITRAN database (Gordon et al 2022).…”

Section: C12 Non-lte Slab Models For Comentioning

confidence: 99%

See 2 more Smart Citations

XUE: Molecular Inventory in the Inner Region of an Extremely Irradiated Protoplanetary Disk

Ramírez-Tannus,

Bik,

Cuijpers

et al. 2023

ApJL

Self Cite

View full text Add to dashboard Cite

We present the first results of the eXtreme UV Environments (XUE) James Webb Space Telescope (JWST) program, which focuses on the characterization of planet-forming disks in massive star-forming regions. These regions are likely representative of the environment in which most planetary systems formed. Understanding the impact of environment on planet formation is critical in order to gain insights into the diversity of the observed exoplanet populations. XUE targets 15 disks in three areas of NGC 6357, which hosts numerous massive OB stars, including some of the most massive stars in our Galaxy. Thanks to JWST, we can, for the first time, study the effect of external irradiation on the inner (<10 au), terrestrial-planet-forming regions of protoplanetary disks. In this study, we report on the detection of abundant water, CO, 12CO2, HCN, and C2H2 in the inner few au of XUE 1, a highly irradiated disk in NGC 6357. In addition, small, partially crystalline silicate dust is present at the disk surface. The derived column densities, the oxygen-dominated gas-phase chemistry, and the presence of silicate dust are surprisingly similar to those found in inner disks located in nearby, relatively isolated low-mass star-forming regions. Our findings imply that the inner regions of highly irradiated disks can retain similar physical and chemical conditions to disks in low-mass star-forming regions, thus broadening the range of environments with similar conditions for inner disk rocky planet formation to the most extreme star-forming regions in our Galaxy.

show abstract

Bending Relaxation of H₂O by Collision with Para‐ and Ortho‐H₂

García‐Vázquez,

Faure,

Stoecklin

2023

ChemPhysChem

View full text Add to dashboard Cite

We extend our recent theoretical work on the bending relaxation of H2O in collisions with H2 by including the three water modes of vibration coupled with rotation, as well as the rotation of H2. Our full quantum close‐coupling method (excluding the H2 vibration) is combined with a high‐accuracy nine‐dimensional potential energy surface. The collisions of para‐H2O and ortho‐H2O with the two spin modifications of H2 are considered and compared for several initial states of H2O. The convergence of the results as a function of the size of the rotational basis set of the two colliders is discussed. In particular, near‐resonant energy transfer between H2O and H2 is found to control the vibrational relaxation process, with a dominant contribution of transitions with = , and being respectively the H2 initial and final rotational quantum numbers. Finally, the calculated value of the H2O bending relaxation rate coefficient at 295 K is found to be in excellent agreement with its experimental estimate.

show abstract

Water in the terrestrial planet-forming zone of the PDS 70 disk

Cited by 16 publications

References 55 publications

A Magnetically Driven Disk Wind in the Inner Disk of PDS 70*

A Magnetically Driven Disk Wind in the Inner Disk of PDS 70*

XUE: Molecular Inventory in the Inner Region of an Extremely Irradiated Protoplanetary Disk

Bending Relaxation of H₂O by Collision with Para‐ and Ortho‐H₂

Contact Info

Product

Resources

About

Water in the terrestrial planet-forming zone of the PDS 70 disk

Cited by 16 publications

References 55 publications

A Magnetically Driven Disk Wind in the Inner Disk of PDS 70*

A Magnetically Driven Disk Wind in the Inner Disk of PDS 70*

XUE: Molecular Inventory in the Inner Region of an Extremely Irradiated Protoplanetary Disk

Bending Relaxation of H2O by Collision with Para‐ and Ortho‐H2

Contact Info

Product

Resources

About

Bending Relaxation of H₂O by Collision with Para‐ and Ortho‐H₂