Planets are formed from the disk of gas and dust around a star, but the mechanisms for doing so are imperfectly understood. Gas is the key driver in the dynamical evolution of planets, for example, because it is the dominant component of the disk (by mass). The timescale over which the gas dissipates sets the timescale for planet formation, yet its distribution in disks is just starting to be carefully measured. Similarly, the chemical composition of the gas determines the composition of the future planets and their atmospheres, but even after decades of studying protoplanetary disks, their chemical compositions are poorly constrained; even the gas-to-dust ratios are largely unknown.
The detailed characterizations of individual sources provide insights into the physical and chemical nature of protoplanetary disks. The star AB Aurigae is a widely studied system hosting a young transitional disk, a disk with gaps suggestive of clearing by newly forming planets. Located 536 light-years (plus-or-minus 1%) from the Sun, it is close enough to be an excellent candidate in which to study the spatial distribution of gas and dust in detail.
CfA astronomer Romane Le Gal was a member of a team that used the NOrthern Extended Millimeter Array (NOEMA) to observe the AB Aur gas disk at high spatial resolution in the emission lines of CO, H2CO, HCN, and SO; combined with archival results, their dataset includes a total of seventeen different spectral features.
The scientists, for the first time in a transition disk, mapped the gas density and the gas-to-dust ratio, finding that it was less than expected — half of the interstellar medium value or even in some places as much as four times smaller. Different molecules were seen tracing different regions of the disk, for instance the envelope or the surface. The team measured the average disk temperature to be about 39K, warmer than estimated in other disks. Not least, their chemical analysis determined the relative abundances of the chemicals and found (depending on some assumptions) that sulfur is strongly depleted compared to the solar system value.
The new paper’s primary conclusion, that the planet-forming disk around this massive young star is significantly different from expectations, highlights the importance of making such detailed observations of disks around massive stars.
Reference: “AB Aur, a Rosetta stone for studies of planet formation I. Chemical study of a planet-forming disk” by P. Rivière-Marichalar, A. Fuente, R. Le Gal, C. Baruteau, R. Neri, D. Navarro-Almaida, S. P. Treviño-Morales, E. Macías, R. Bachiller and M. Osorio, 1 October 2020, Astronomy & Astrophysics.
DOI: 10.1051/0004-6361/202038549
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3 Comments
“The scientists, for the first time in a transition disk, mapped the gas density and the gas-to-dust ratio, finding that it was less than expected — half of the interstellar medium value or even in some places as much as four times smaller.”
May refer to:
“5.- The derived gas-to-dust ratios along the central parts of the dust ring range from ∼ 10 to ∼ 40, and reach 200 only in the inner and outer edges. As expected, the minimum gas-to-dust ratio is measured towards the dust trap. This value of the gas-to-dust ratio is in agreement with values typically found in T Tauri and Herbig Ae/Be disks.”
On the dust ring the paper says:
“Dust trapping in local pressure maxima has been proposed to overcome the radial drift of solid particles, and hence favor planet formation in transitions disks.”
I.e. it could confirm that a planet and its formation process sops up gas (early on).
Here we go making things up from one little bit of fact. Omg, give it a rest and do your jobs and quit gossiping. You ruin any reputation you have.