AB Aur, a Rosetta stone for studies of planet formation. I. Chemical study of a planet-forming disk

DOI: 
10.1051/0004-6361/202038549
Publication date: 
01/10/2020
Main author: 
Rivière-Marichalar, P.
IAA authors: 
Osorio, M.
Authors: 
Rivière-Marichalar, P.;Fuente, A.;Le Gal, R.;Baruteau, C.;Neri, R.;Navarro-Almaida, D.;Treviño-Morales, S. P.;Macías, E.;Bachiller, R.;Osorio, M.
Journal: 
Astronomy and Astrophysics
Refereed: 
Yes
Publication type: 
Article
Volume: 
642
Pages: 
A32
Abstract: 
Context. AB Aur is a Herbig Ae star that hosts a prototypical transition disk. The disk shows a plethora of features connected with planet formation mechanisms, such as spiral arms, dust cavities, and dust traps. Understanding the physical and chemical characteristics of these features is crucial to advancing our knowledge of the planet formation processes. <BR /> Aims: We aim to characterize the gaseous disk around the Herbig Ae star AB Aur. A complete spectroscopic study was performed using NOEMA to determine the physical and chemical conditions with high spatial resolution. <BR /> Methods: We present new NOrthern Extended Millimeter Array (NOEMA) interferometric observations of the continuum and <SUP>12</SUP>CO, <SUP>13</SUP>CO, C<SUP>18</SUP>O, H<SUB>2</SUB>CO, and SO lines obtained at high resolution. We used the integrated intensity maps and stacked spectra to derive reliable estimates of the disk temperature. By combining our <SUP>13</SUP>CO and C<SUP>18</SUP>O observations, we computed the gas-to-dust ratio along the disk. We also derived column density maps for the different species and used them to compute abundance maps. The results of our observations were compared with a set of Nautilus astrochemical models to obtain insight into the disk properties. <BR /> Results: We detected continuum emission in a ring that extends from 0.6'' to ~2.0'', peaking at 0.97'' and with a strong azimuthal asymmetry. The molecules observed show different spatial distributions, and the peaks of the distributions are not correlated with the binding energy. Using H<SUB>2</SUB>CO and SO lines, we derived a mean disk temperature of 39 K. We derived a gas-to-dust ratio that ranges from 10 to 40 along the disk. Abundance with respect to <SUP>13</SUP>CO for SO (~2 × 10<SUP>-4</SUP>) is almost one order of magnitude greater than the value derived for H<SUB>2</SUB>CO (1.6 × 10<SUP>-5</SUP>). The comparison with Nautilus models favors a disk with a low gas-to-dust ratio (40) and prominent sulfur depletion. <BR /> Conclusions: From a very complete spectroscopic study of the prototypical disk around AB Aur, we derived, for the first time, the gas temperature and the gas-to-dust ratio along the disk, providing information that is essential to constraining hydrodynamical simulations. Moreover, we explored the gas chemistry and, in particular, the sulfur depletion. The derived sulfur depletion is dependent on the assumed C/O ratio. Our data are better explained with C/O ~ 0.7 and S/H = 8 × 10<SUP>-8</SUP>.
Database: 
ADS
SCOPUS
URL: 
https://ui.adsabs.harvard.edu/#abs/2020A&A...642A..32R/abstract
ADS Bibcode: 
2020A&A...642A..32R
Keywords: 
astrochemistry;protoplanetary disks;planet-disk interactions;stars: variables: T Tauri;Herbig Ae/Be;radio continuum: stars;radio lines: planetary systems;Astrophysics - Solar and Stellar Astrophysics;Astrophysics - Earth and Planetary Astrophysics;Astrophysics - Astrophysics of Galaxies