A far-ultraviolet-driven photoevaporation flow observed in a protoplanetary disk
Most low-mass stars form in stellar clusters that also contain massive stars, which are sources of far-ultraviolet (FUV) radiation. Theoretical models predict that this FUV radiation produces photo-dissociation regions (PDRs) on the surfaces of protoplanetary disks around low-mass stars, impacting planet formation within the disks. We report JWST and Atacama Large Millimetere Array observations of a FUV-irradiated protoplanetary disk in the Orion Nebula. Emission lines are detected from the PDR; modelling their kinematics and excitation allows us to constrain the physical conditions within the gas. We quantify the mass-loss rate induced by the FUV irradiation, finding it is sufficient to remove gas from the disk in less than a million years. This is rapid enough to affect giant planet formation in the disk..
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Preprint| Erscheinungsjahr: |
2024 |
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| Erschienen: |
2024 |
| Enthalten in: |
arXiv.org - (2024) vom: 29. Feb. Zur Gesamtaufnahme - year:2024 |
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| Sprache: |
Englisch |
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| Links: |
Volltext [kostenfrei] |
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| PPN (Katalog-ID): |
XCH042744148 |
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| 100 | 1 | |a Berné, Olivier |e verfasserin |4 aut | |
| 245 | 1 | 0 | |a A far-ultraviolet-driven photoevaporation flow observed in a protoplanetary disk |
| 264 | 1 | |c 2024 | |
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| 337 | |a Computermedien |b c |2 rdamedia | ||
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| 520 | |a Most low-mass stars form in stellar clusters that also contain massive stars, which are sources of far-ultraviolet (FUV) radiation. Theoretical models predict that this FUV radiation produces photo-dissociation regions (PDRs) on the surfaces of protoplanetary disks around low-mass stars, impacting planet formation within the disks. We report JWST and Atacama Large Millimetere Array observations of a FUV-irradiated protoplanetary disk in the Orion Nebula. Emission lines are detected from the PDR; modelling their kinematics and excitation allows us to constrain the physical conditions within the gas. We quantify the mass-loss rate induced by the FUV irradiation, finding it is sufficient to remove gas from the disk in less than a million years. This is rapid enough to affect giant planet formation in the disk. | ||
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| 773 | 0 | 8 | |i Enthalten in |t arXiv.org |g (2024) vom: 29. Feb. |
| 773 | 1 | 8 | |g year:2024 |g day:29 |g month:02 |
| 856 | 4 | 0 | |u https://arxiv.org/abs/2403.00160 |z kostenfrei |3 Volltext |
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| 952 | |j 2024 |b 29 |c 02 | ||