JWST-DECO: The Impact of Accretion on Mid-Infrared Observable Water in Planet-forming Disks
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2026
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| author | Calahan, Jenny K. Dziire, Tarisai Öberg, Karin Banzatti, Andrea Cleeves, L. Ilsedore Alarcón, Felipe Blake, Geoffrey A. Colmenares, María José González-Ruilova, Camilo Gupta, Aashish Hernández-Vera, Claudio Kaeufer, Till Krijt, Sebastiaan Law, Charles J. Molyarova, Tamara Williams, Joe |
| author_facet | Calahan, Jenny K. Dziire, Tarisai Öberg, Karin Banzatti, Andrea Cleeves, L. Ilsedore Alarcón, Felipe Blake, Geoffrey A. Colmenares, María José González-Ruilova, Camilo Gupta, Aashish Hernández-Vera, Claudio Kaeufer, Till Krijt, Sebastiaan Law, Charles J. Molyarova, Tamara Williams, Joe |
| contents | The inner few au of a protoplanetary disk hosts the majority of observed exoplanets and is the primary planet-forming zone of the disk. The mid-IR spectra of disks, with its rich forest of water lines, provides key insights into the composition of forming planets. One of the strongest trends seen with data from Spitzer and now JWST is a correlation between the increase in water line flux and accretion luminosity of a system. We set out to reproduce and understand this trend by adding an accretion module to the thermo-chemical code DALI, and explore how viscous accretion heating and the addition of accretion luminosity impacts the 2D temperature structure and the observable water reservoir. We reproduce the trend that the observed water mass increases with accretion rate, with hot, warm, and cool water being more to less strongly correlated, respectively. Our model suggests that these trends are due to an increased emitting area with accretion rate, with some of the cool and warm population becoming hidden underneath an optically thick dust surface and being constrained to a smaller disk volume. This trend is driven by the accretion-related increase in central luminosity, while viscous heating centralized to the midplane has no impact on observed water mass. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2605_22926 |
| institution | arXiv |
| publishDate | 2026 |
| record_format | arxiv |
| spellingShingle | JWST-DECO: The Impact of Accretion on Mid-Infrared Observable Water in Planet-forming Disks Calahan, Jenny K. Dziire, Tarisai Öberg, Karin Banzatti, Andrea Cleeves, L. Ilsedore Alarcón, Felipe Blake, Geoffrey A. Colmenares, María José González-Ruilova, Camilo Gupta, Aashish Hernández-Vera, Claudio Kaeufer, Till Krijt, Sebastiaan Law, Charles J. Molyarova, Tamara Williams, Joe Earth and Planetary Astrophysics Solar and Stellar Astrophysics The inner few au of a protoplanetary disk hosts the majority of observed exoplanets and is the primary planet-forming zone of the disk. The mid-IR spectra of disks, with its rich forest of water lines, provides key insights into the composition of forming planets. One of the strongest trends seen with data from Spitzer and now JWST is a correlation between the increase in water line flux and accretion luminosity of a system. We set out to reproduce and understand this trend by adding an accretion module to the thermo-chemical code DALI, and explore how viscous accretion heating and the addition of accretion luminosity impacts the 2D temperature structure and the observable water reservoir. We reproduce the trend that the observed water mass increases with accretion rate, with hot, warm, and cool water being more to less strongly correlated, respectively. Our model suggests that these trends are due to an increased emitting area with accretion rate, with some of the cool and warm population becoming hidden underneath an optically thick dust surface and being constrained to a smaller disk volume. This trend is driven by the accretion-related increase in central luminosity, while viscous heating centralized to the midplane has no impact on observed water mass. |
| title | JWST-DECO: The Impact of Accretion on Mid-Infrared Observable Water in Planet-forming Disks |
| topic | Earth and Planetary Astrophysics Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2605.22926 |