CO gaps in cold transition disks around low-mass stars
Authors: A. A. Rota (Leiden Observatory, the Netherlands), N. van der Marel (Leiden Observatory, the Netherlands), E. F. van Dishoeck (Leiden Observatory, the Netherlands), T. Muto (Kogakuin University, Japan)
Abstract
Transition disks with large inner dust cavities are promising targets to study planet formation, as these disks are likely hosting massive planetary companions. The structure of gas and dust inside the cavity are crucial for understanding the potential of planet formation in the regions. We investigate the structure of gas and dust in a sample of three cold, inclined transition disks around K and M stars without evidence for an inner dusty disk. We present new high-resolution ALMA Band 6 data of both 230 GHz continuum at 0.02" (~3 au) resolution and the 12CO 2-1, 13CO 2-1, C18O 2-1 isotopologues at 0.12" (~20 au) resolution. We analyze the radial profiles, compute the brightness temperatures, and derive estimates of the gas and dust content of the inner disk at 1 au. All three disks show dust cavities of 30-40 au in radius. The CO emission extends inside the cavity with progressively smaller CO cavity radii for the more abundant isotopologues. The 13CO brightness temperature profile is similar to that of other transition disks and full disks. No inner dust disk is detected in the ALMA continuum, consistent with the lack of near-infrared excess. Considering the accretion rates, the gas-to-dust ratio in the inner disk at 1 au is estimated to be as high as 10^5. No significant differences in the brightness temperature or in the gas-to-dust ratio are found between our disks and other transition disks around more luminous stars, contrary to expectations. This highlights the importance of individual-target studies through thermochemical modeling or multi-transition analyses to constrain the dust and gas structures in the cavity. The observed disk structures could be explained by super-Jovian companion on eccentric orbits, but further modeling is needed to confirm this conclusion.
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Abstract
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This study uses ALMA and NOEMA CO-isotopologue lines to estimate gas mass in a protoplanetary disk, rather than mapping transition-disk cavities.
In short
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Abstract
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Abstract
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In short
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Abstract
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Abstract
We present ISO-SWS observations of H2 pure-rotational line emission from the disks around low and intermediate mass pre-main-sequence stars as well as from young stars thought to be surrounded by debris disks. We detect `warm' (T ~ 100-200 K) H2 gas around many sources, including tentatively the debris-disk objects. The mass of this warm gas ranges from ~1E-4 Solar mass up to 8E-3 Solar mass, and can constitute a non-negligible fraction of the total disk mass. Complementary single-dish 12CO 3-2, 13CO 3-2 and 12CO 6-5 observations have been obtained as well. These transitions probe cooler gas at T ~ 20-80 K. Most objects show a double-peaked CO emission profile characteristic of a disk in Kep…
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Thermochemical constraints on a primordial-origin of gas-rich debris disksH. Mitani, W. Ooyama, R. Nakatani et al. · 2026 · arXiv (Cornell University) preprint · AI summary available
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In short
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