MINDS. Cha Hα 1, a brown dwarf with a hydrocarbon-rich disk
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| Format: | Preprint |
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2025
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| author | Morales-Calderón, María Jang, Hyerin Arabhavi, Aditya M. Christiaens, Valentin Barrado, David Kamp, Inga van Dishoeck, Ewine F. Henning, Thomas Waters, L. B. F. M. Temmink, Milou Güdel, Manuel Lagage, Pierre-Olivier Garatti, Alessio Caratti o Glauser, Adrian M. Ray, Tom P. Franceschi, Riccardo Gasman, Danny Grant, Sierra L. Kaeufer, Till Kanwar, Jayatee Perotti, Giulia Samland, Matthias Schwarz, Kamber Vlasblom, Marissa Colina, Luis Östlin, Göran |
| author_facet | Morales-Calderón, María Jang, Hyerin Arabhavi, Aditya M. Christiaens, Valentin Barrado, David Kamp, Inga van Dishoeck, Ewine F. Henning, Thomas Waters, L. B. F. M. Temmink, Milou Güdel, Manuel Lagage, Pierre-Olivier Garatti, Alessio Caratti o Glauser, Adrian M. Ray, Tom P. Franceschi, Riccardo Gasman, Danny Grant, Sierra L. Kaeufer, Till Kanwar, Jayatee Perotti, Giulia Samland, Matthias Schwarz, Kamber Vlasblom, Marissa Colina, Luis Östlin, Göran |
| contents | Context. Recent JWST observations have shown that brown dwarfs (BD) are chemically rich, offering valuable insights into giant planet formation. Aims. As part of the MIRI mid-INfrared Disk Survey (MINDS) JWST guaranteed time program, we aim to characterize the gas and dust composition of the disk around the brown dwarf [NC98] Cha HA 1, hereafter Cha H$α$ 1, in the mid-infrared. Methods. We obtain data from the MIRI Medium Resolution Spectrometer (MRS) from 4.9 to 28$μ$m. We use the dust fitting tool DuCK to investigate the dust composition and grain sizes while we identify and fit molecular emission using slab models. Results. Compared with disks around very low mass stars, clear silicate emission features are seen in this BD disk. In addition, JWST reveals a plethora of hydrocarbons, including C$_2$H$_2$, $^{13}$CCH$_2$, CH$_3$, CH$_4$, C$_2$H$_4$, C$_4$H$_2$, C$_3$H$_4$, C$_2$H$_6$, and C$_6$H$_6$ which suggest a disk with a gas C/O > 1. Additionally, we detect CO$_2$, $^{13}$CO$_2$, HCN, H$_2$, and H$_2$O. CO and OH are absent from the spectrum. The dust is dominated by large $\sim$4 $μ$m size amorphous silicates (MgSiO$_3$). We infer a small dust mass fraction ($>$10$\%$) of 5 $μ$m size crystalline forsterite. We do not detect polycyclic aromatic hydrocarbons. Conclusions. Cha H$α$ 1 shows the most diverse chemistry seen to date in a BD protoplanetary disk, consisting of a strong dust feature, 12 carbon-bearing molecules plus H$_2$, and water. The diverse molecular environment offers a unique opportunity to test our understanding of BD disks chemistry and how it affects the possible planets forming in them. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2508_05155 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | MINDS. Cha Hα 1, a brown dwarf with a hydrocarbon-rich disk Morales-Calderón, María Jang, Hyerin Arabhavi, Aditya M. Christiaens, Valentin Barrado, David Kamp, Inga van Dishoeck, Ewine F. Henning, Thomas Waters, L. B. F. M. Temmink, Milou Güdel, Manuel Lagage, Pierre-Olivier Garatti, Alessio Caratti o Glauser, Adrian M. Ray, Tom P. Franceschi, Riccardo Gasman, Danny Grant, Sierra L. Kaeufer, Till Kanwar, Jayatee Perotti, Giulia Samland, Matthias Schwarz, Kamber Vlasblom, Marissa Colina, Luis Östlin, Göran Solar and Stellar Astrophysics Earth and Planetary Astrophysics Context. Recent JWST observations have shown that brown dwarfs (BD) are chemically rich, offering valuable insights into giant planet formation. Aims. As part of the MIRI mid-INfrared Disk Survey (MINDS) JWST guaranteed time program, we aim to characterize the gas and dust composition of the disk around the brown dwarf [NC98] Cha HA 1, hereafter Cha H$α$ 1, in the mid-infrared. Methods. We obtain data from the MIRI Medium Resolution Spectrometer (MRS) from 4.9 to 28$μ$m. We use the dust fitting tool DuCK to investigate the dust composition and grain sizes while we identify and fit molecular emission using slab models. Results. Compared with disks around very low mass stars, clear silicate emission features are seen in this BD disk. In addition, JWST reveals a plethora of hydrocarbons, including C$_2$H$_2$, $^{13}$CCH$_2$, CH$_3$, CH$_4$, C$_2$H$_4$, C$_4$H$_2$, C$_3$H$_4$, C$_2$H$_6$, and C$_6$H$_6$ which suggest a disk with a gas C/O > 1. Additionally, we detect CO$_2$, $^{13}$CO$_2$, HCN, H$_2$, and H$_2$O. CO and OH are absent from the spectrum. The dust is dominated by large $\sim$4 $μ$m size amorphous silicates (MgSiO$_3$). We infer a small dust mass fraction ($>$10$\%$) of 5 $μ$m size crystalline forsterite. We do not detect polycyclic aromatic hydrocarbons. Conclusions. Cha H$α$ 1 shows the most diverse chemistry seen to date in a BD protoplanetary disk, consisting of a strong dust feature, 12 carbon-bearing molecules plus H$_2$, and water. The diverse molecular environment offers a unique opportunity to test our understanding of BD disks chemistry and how it affects the possible planets forming in them. |
| title | MINDS. Cha Hα 1, a brown dwarf with a hydrocarbon-rich disk |
| topic | Solar and Stellar Astrophysics Earth and Planetary Astrophysics |
| url | https://arxiv.org/abs/2508.05155 |