JWST Ice Band Profiles Reveal Mixed Ice Compositions in the HH 48 NE Disk

Planet formation is strongly influenced by the composition and distribution of volatiles within protoplanetary disks. With JWST, it is now possible to obtain direct observational constraints on disk ices, as recently demonstrated by the detection of ice absorption features toward the edge-on HH 48 N...

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Published in:The Astrophysical journal 2024-11, Vol.975 (2), p.166
Main Authors: Bergner, Jennifer B., Sturm, J. A., Piacentino, Elettra L., McClure, M. K., Öberg, Karin I., Boogert, A. C. A., Dartois, E., Drozdovskaya, M. N., Fraser, H. J., Harsono, Daniel, Ioppolo, Sergio, Law, Charles J., Lis, Dariusz C., McGuire, Brett A., Melnick, Gary J., Noble, Jennifer A., Palumbo, M. E., Pendleton, Yvonne J., Perotti, Giulia, Qasim, Danna, Rocha, W. R. M., van Dishoeck, E. F.
Format: Article
Language:English
Subjects:
Accretion disks
Astrochemistry
Carbon dioxide
Entrapment
Ice ages
Ice composition
Ice formation
Interstellar molecules
Planet formation
Planetary composition
Planetary evolution
Protoplanetary disks
Protostars
Radiative transfer
Reprocessing
Star formation
Stellar evolution
Volatile compounds
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Summary:Planet formation is strongly influenced by the composition and distribution of volatiles within protoplanetary disks. With JWST, it is now possible to obtain direct observational constraints on disk ices, as recently demonstrated by the detection of ice absorption features toward the edge-on HH 48 NE disk as part of the Ice Age Early Release Science program. Here, we introduce a new radiative transfer modeling framework designed to retrieve the composition and mixing status of disk ices using their band profiles, and apply it to interpret the H 2 O, CO 2 , and CO ice bands observed toward the HH 48 NE disk. We show that the ices are largely present as mixtures, with strong evidence for CO trapping in both H 2 O and CO 2 ice. The HH 48 NE disk ice composition (pure versus polar versus apolar fractions) is markedly different from earlier protostellar stages, implying thermal and/or chemical reprocessing during the formation or evolution of the disk. We infer low ice-phase C/O ratios around 0.1 throughout the disk, and also demonstrate that the mixing and entrapment of disk ices can dramatically affect the radial dependence of the C/O ratio. It is therefore imperative that realistic disk ice compositions are considered when comparing planetary compositions with potential formation scenarios, which will fortunately be possible for an increasing number of disks with JWST.
ISSN:0004-637X
1538-4357
DOI:10.3847/1538-4357/ad79fc