XUE: Thermochemical Modeling Suggests a Compact and Gas-depleted Structure for a Distant, Irradiated Protoplanetary Disk
Unveiling the physical structure of protoplanetary disks is crucial for interpreting the diversity of the exoplanet population. Until recently, the census of the physical properties of protoplanetary disks probed by mid-infrared observations was limited to the solar neighborhood ( d ≲ 250 pc). Howe...
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IOP Publishing
2025-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/adc91d |
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| author | Bayron Portilla-Revelo Konstantin V. Getman María Claudia Ramírez-Tannus Thomas J. Haworth Rens Waters Arjan Bik Eric D. Feigelson Inga Kamp Sierk E. van Terwisga Jenny Frediani Thomas Henning Andrew J. Winter Veronica Roccatagliata Thomas Preibisch E. Sabbi Peter Zeidler Michael A. Kuhn |
| author_facet | Bayron Portilla-Revelo Konstantin V. Getman María Claudia Ramírez-Tannus Thomas J. Haworth Rens Waters Arjan Bik Eric D. Feigelson Inga Kamp Sierk E. van Terwisga Jenny Frediani Thomas Henning Andrew J. Winter Veronica Roccatagliata Thomas Preibisch E. Sabbi Peter Zeidler Michael A. Kuhn |
| author_sort | Bayron Portilla-Revelo |
| collection | DOAJ |
| description | Unveiling the physical structure of protoplanetary disks is crucial for interpreting the diversity of the exoplanet population. Until recently, the census of the physical properties of protoplanetary disks probed by mid-infrared observations was limited to the solar neighborhood ( d ≲ 250 pc). However, nearby star-forming regions (SFRs) such as Taurus—where no O-type stars reside—are not representative of the environments where the majority of the planet formation occurs in the Galaxy. The James Webb Space Telescope (JWST) now enables observations of disks in distant high-mass SFRs, where strong external far-ultraviolet radiation is expected to impact those disks. Nevertheless, a detailed characterization of the population of externally irradiated disks is still lacking. We use the thermochemical code ProDiMo to model JWST/MIRI spectroscopy and archival visual/near-infrared photometry aiming to constrain the physical structure of the irradiated disk around the solar-mass star XUE 1 in NGC 6357 ( d ≈ 1690 pc). Our findings are as follows. (1) Mid-infrared dust emission features are explained by amorphous and crystalline silicates with compositions similar to nearby disks. (2) The molecular features detected with MIRI originate within the first ∼1 au, consistent with results from slab models. (3) Our model favors a disk truncated at 10 au with a gas-to-dust ratio of unity in the outskirts. (4) Comparing models of the same disk structure under different irradiation levels, we find that strong external irradiation raises gas temperature tenfold and boosts water abundance beyond 10 au by a factor of 100. |
| format | Article |
| id | doaj-art-6cdb98766d714ea194abbd564a96b33b |
| institution | OA Journals |
| issn | 1538-4357 |
| language | English |
| publishDate | 2025-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj-art-6cdb98766d714ea194abbd564a96b33b2025-08-20T02:32:46ZengIOP PublishingThe Astrophysical Journal1538-43572025-01-0198517210.3847/1538-4357/adc91dXUE: Thermochemical Modeling Suggests a Compact and Gas-depleted Structure for a Distant, Irradiated Protoplanetary DiskBayron Portilla-Revelo0https://orcid.org/0000-0002-6278-9006Konstantin V. Getman1https://orcid.org/0000-0002-6137-8280María Claudia Ramírez-Tannus2https://orcid.org/0000-0001-9698-4080Thomas J. Haworth3https://orcid.org/0000-0002-9593-7618Rens Waters4https://orcid.org/0000-0002-5462-9387Arjan Bik5https://orcid.org/0000-0001-8068-0891Eric D. Feigelson6https://orcid.org/0000-0002-5077-6734Inga Kamp7https://orcid.org/0000-0001-7455-5349Sierk E. van Terwisga8https://orcid.org/0000-0002-1284-5831Jenny Frediani9https://orcid.org/0009-0003-7663-5280Thomas Henning10https://orcid.org/0000-0002-1493-300XAndrew J. Winter11https://orcid.org/0000-0002-7501-9801Veronica Roccatagliata12https://orcid.org/0000-0002-4650-594XThomas Preibisch13https://orcid.org/0000-0003-3130-7796E. Sabbi14https://orcid.org/0000-0003-2954-7643Peter Zeidler15https://orcid.org/0000-0002-6091-7924Michael A. Kuhn16https://orcid.org/0000-0002-0631-7514Department of Astronomy and Astrophysics, The Pennsylvania State University , 525 Davey Laboratory, University Park, PA 16802, USA ; bmp5924@psu.edu; Center for Exoplanets and Habitable Worlds, Penn State University , 525 Davey Laboratory, 251 Pollock Road, University Park, PA 16802, USADepartment of Astronomy and Astrophysics, The Pennsylvania State University , 525 Davey Laboratory, University Park, PA 16802, USA ; bmp5924@psu.eduMax-Planck Institut für Astronomie (MPIA) , Königstuhl 17, D-69117 Heidelberg, GermanyAstronomy Unit, School of Physics and Astronomy, Queen Mary University of London , London, E1 4NS, UKDepartment of Astrophysics/IMAPP, Radboud University , PO Box 9010, 6500 GL Nijmegen, The Netherlands; SRON Netherlands Institute for Space Research , Niels Bohrweg 4, NL-2333 CA Leiden, The NetherlandsDepartment of Astronomy, Stockholm University , AlbaNova University Center, SE-10691 Stockholm, SwedenDepartment of Astronomy and Astrophysics, The Pennsylvania State University , 525 Davey Laboratory, University Park, PA 16802, USA ; bmp5924@psu.edu; Center for Astrostatistics, Pennsylvania State University , 517 Thomas Building, University Park, PA 16802, USAKapteyn Astronomical Institute, University of Groningen , PO BOX 800, 9700 AV Groningen, The NetherlandsSpace Research Institute , Austrian Academy of Sciences, Schmiedlstr. 6, 8042, Graz, AustriaDepartment of Astronomy, Stockholm University , AlbaNova University Center, SE-10691 Stockholm, SwedenMax-Planck Institut für Astronomie (MPIA) , Königstuhl 17, D-69117 Heidelberg, GermanyMax-Planck Institut für Astronomie (MPIA) , Königstuhl 17, D-69117 Heidelberg, Germany; Université Côte d’Azur , Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange, 06300 Nice, FranceDipartimento di Fisica e Astronomia, Alma Mater Studiorum, Universitàdi Bologna , Via Gobetti 93/2, I-40129 Bologna, Italy; INAF-Osservatorio Astrofisico di Arcetri , Largo E. Fermi 5, I-50125 Firenze, ItalyUniversitäts-Sternwarte München , Ludwig-Maximilians-Universität, Scheinerstr. 1, 81679 München, GermanyGemini Observatory/NSFs NOIRLab , 950 N. Cherry Avenue, Tucson, AZ 85719, USAAURA for the European Space Agency (ESA), ESA Office, Space Telescope Science Institute , 3700 San Martin Drive, Baltimore, MD 21218, USACentre for Astrophysics Research, Department of Physics, Astronomy and Mathematics, University of Hertfordshire , Hatfield, AL10 9AB, UKUnveiling the physical structure of protoplanetary disks is crucial for interpreting the diversity of the exoplanet population. Until recently, the census of the physical properties of protoplanetary disks probed by mid-infrared observations was limited to the solar neighborhood ( d ≲ 250 pc). However, nearby star-forming regions (SFRs) such as Taurus—where no O-type stars reside—are not representative of the environments where the majority of the planet formation occurs in the Galaxy. The James Webb Space Telescope (JWST) now enables observations of disks in distant high-mass SFRs, where strong external far-ultraviolet radiation is expected to impact those disks. Nevertheless, a detailed characterization of the population of externally irradiated disks is still lacking. We use the thermochemical code ProDiMo to model JWST/MIRI spectroscopy and archival visual/near-infrared photometry aiming to constrain the physical structure of the irradiated disk around the solar-mass star XUE 1 in NGC 6357 ( d ≈ 1690 pc). Our findings are as follows. (1) Mid-infrared dust emission features are explained by amorphous and crystalline silicates with compositions similar to nearby disks. (2) The molecular features detected with MIRI originate within the first ∼1 au, consistent with results from slab models. (3) Our model favors a disk truncated at 10 au with a gas-to-dust ratio of unity in the outskirts. (4) Comparing models of the same disk structure under different irradiation levels, we find that strong external irradiation raises gas temperature tenfold and boosts water abundance beyond 10 au by a factor of 100.https://doi.org/10.3847/1538-4357/adc91dStar forming regionsPlanet formationProtoplanetary disksInfrared spectroscopyRadiative transfer simulations |
| spellingShingle | Bayron Portilla-Revelo Konstantin V. Getman María Claudia Ramírez-Tannus Thomas J. Haworth Rens Waters Arjan Bik Eric D. Feigelson Inga Kamp Sierk E. van Terwisga Jenny Frediani Thomas Henning Andrew J. Winter Veronica Roccatagliata Thomas Preibisch E. Sabbi Peter Zeidler Michael A. Kuhn XUE: Thermochemical Modeling Suggests a Compact and Gas-depleted Structure for a Distant, Irradiated Protoplanetary Disk The Astrophysical Journal Star forming regions Planet formation Protoplanetary disks Infrared spectroscopy Radiative transfer simulations |
| title | XUE: Thermochemical Modeling Suggests a Compact and Gas-depleted Structure for a Distant, Irradiated Protoplanetary Disk |
| title_full | XUE: Thermochemical Modeling Suggests a Compact and Gas-depleted Structure for a Distant, Irradiated Protoplanetary Disk |
| title_fullStr | XUE: Thermochemical Modeling Suggests a Compact and Gas-depleted Structure for a Distant, Irradiated Protoplanetary Disk |
| title_full_unstemmed | XUE: Thermochemical Modeling Suggests a Compact and Gas-depleted Structure for a Distant, Irradiated Protoplanetary Disk |
| title_short | XUE: Thermochemical Modeling Suggests a Compact and Gas-depleted Structure for a Distant, Irradiated Protoplanetary Disk |
| title_sort | xue thermochemical modeling suggests a compact and gas depleted structure for a distant irradiated protoplanetary disk |
| topic | Star forming regions Planet formation Protoplanetary disks Infrared spectroscopy Radiative transfer simulations |
| url | https://doi.org/10.3847/1538-4357/adc91d |
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