Abstract:

Infrared observations of the inner disks around very low-mass stars (VLMS; <0.3 M_⊙) have revealed a carbon-rich gas composition in the terrestrial planet-forming regions. Contrary to the typically water-rich T Tauri disk spectra, only two disks around VLMS have been observed to be water-rich among more than 10 VLMS disks observed so far with JWST/MIRI. In this Letter, we systematically search for the presence of water and other oxygen-bearing molecules in the JWST/MIRI spectra of 10 VLMS disks from the MIRI mid-INfrared Disk Survey (MINDS). In addition to the two previously reported detections of water emission in this VLMS sample, we detect water emission in the spectra of three other sources and tentatively in one source, and we provide strong evidence for water emission in the remaining disks in the MINDS sample, most of which have bright emission from carbon-bearing molecules. We show that the C₂H₂ emission is much stronger than that of water for sources with low luminosities, and the hydrocarbons outshine the water emission in such conditions. We propose that the appearance of water-rich versus hydrocarbon-rich spectra is related to the location of the water reservoir in the disk relative to the main hydrocarbon reservoir. Our findings indicate that the terrestrial planet-forming regions in VLMS disks have high carbon-to-oxygen ratios (C/O > 1) but can still harbor ample water, similar to those in the T Tauri disks.

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