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| Autores principales: | , , , , , , , , , , , , , , , , |
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| Formato: | Preprint |
| Publicado: |
2024
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| Materias: | |
| Acceso en línea: | https://arxiv.org/abs/2407.05070 |
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| _version_ | 1866916314169212928 |
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| author | Temmink, Milou van Dishoeck, Ewine F. Gasman, Danny Grant, Sierra L. Tabone, Benoit Guedel, Manuel Henning, Thomas Barrado, David Garatti, Alessio Caratti o Glauser, Adrian M. Kamp, Inga Arabhavi, Aditya M. Jang, Hyerin Kurtovic, Nicolas Perotti, Giulia Schwarz, Kamber Vlasblom, Marissa |
| author_facet | Temmink, Milou van Dishoeck, Ewine F. Gasman, Danny Grant, Sierra L. Tabone, Benoit Guedel, Manuel Henning, Thomas Barrado, David Garatti, Alessio Caratti o Glauser, Adrian M. Kamp, Inga Arabhavi, Aditya M. Jang, Hyerin Kurtovic, Nicolas Perotti, Giulia Schwarz, Kamber Vlasblom, Marissa |
| contents | The MRS mode of the JWST-MIRI instrument gives insights into the chemical richness and complexity of the inner regions of planet-forming disks. Here, we analyse the H$_2$O-rich spectrum of the compact disk DR Tau. We probe the excitation conditions of the H$_2$O transitions observed in different wavelength regions across the entire spectrum using LTE slab models, probing both the rovibrational and rotational transitions. These regions suggest a radial temperature gradient, as the excitation temperature (emitting radius) decreases (increases) with increasing wavelength. To explain the derived emitting radii, we require a larger inclination for the inner disk (i~20-23 degrees) compared to the outer disk (i~5 degrees), agreeing with our previous analysis on CO. We also analyse the pure rotational spectrum (<10 micron) using a large, structured disk (CI Tau) as a template, confirming the presence of the radial gradient, and by fitting multiple components to further characterise the radial and vertical temperature gradients present in the spectrum. At least three temperature components (T~180-800 K) are required to reproduce the rotational spectrum of H$_2$O arising from the inner ~0.3-8 au. These components describe a radial temperature gradient that scales roughly as ~R$^{-0.5}$ in the emitting layers. As the H$_2$O is mainly optically thick, we derive a lower limit on the abundance ratio of H$_2$O/CO~0.17, suggesting a potential depletion of H$_2$O. Similarly to previous work, we detect a cold H$_2$O component (T~180 K) originating from near the snowline. We cannot conclude if an enhancement of the H$_2$O reservoir is observed following radial drift. A consistent analysis of a larger sample of compact disks is necessary to study the importance of drift in enhancing the H$_2$O abundances. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2407_05070 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | MINDS. The DR Tau disk II: probing the hot and cold H$_2$O reservoirs in the JWST-MIRI spectrum Temmink, Milou van Dishoeck, Ewine F. Gasman, Danny Grant, Sierra L. Tabone, Benoit Guedel, Manuel Henning, Thomas Barrado, David Garatti, Alessio Caratti o Glauser, Adrian M. Kamp, Inga Arabhavi, Aditya M. Jang, Hyerin Kurtovic, Nicolas Perotti, Giulia Schwarz, Kamber Vlasblom, Marissa Earth and Planetary Astrophysics The MRS mode of the JWST-MIRI instrument gives insights into the chemical richness and complexity of the inner regions of planet-forming disks. Here, we analyse the H$_2$O-rich spectrum of the compact disk DR Tau. We probe the excitation conditions of the H$_2$O transitions observed in different wavelength regions across the entire spectrum using LTE slab models, probing both the rovibrational and rotational transitions. These regions suggest a radial temperature gradient, as the excitation temperature (emitting radius) decreases (increases) with increasing wavelength. To explain the derived emitting radii, we require a larger inclination for the inner disk (i~20-23 degrees) compared to the outer disk (i~5 degrees), agreeing with our previous analysis on CO. We also analyse the pure rotational spectrum (<10 micron) using a large, structured disk (CI Tau) as a template, confirming the presence of the radial gradient, and by fitting multiple components to further characterise the radial and vertical temperature gradients present in the spectrum. At least three temperature components (T~180-800 K) are required to reproduce the rotational spectrum of H$_2$O arising from the inner ~0.3-8 au. These components describe a radial temperature gradient that scales roughly as ~R$^{-0.5}$ in the emitting layers. As the H$_2$O is mainly optically thick, we derive a lower limit on the abundance ratio of H$_2$O/CO~0.17, suggesting a potential depletion of H$_2$O. Similarly to previous work, we detect a cold H$_2$O component (T~180 K) originating from near the snowline. We cannot conclude if an enhancement of the H$_2$O reservoir is observed following radial drift. A consistent analysis of a larger sample of compact disks is necessary to study the importance of drift in enhancing the H$_2$O abundances. |
| title | MINDS. The DR Tau disk II: probing the hot and cold H$_2$O reservoirs in the JWST-MIRI spectrum |
| topic | Earth and Planetary Astrophysics |
| url | https://arxiv.org/abs/2407.05070 |