Chemical evolution during the formation of a protoplanetary disk

Abstract

(Abridged) The aim of this study is to investigate the chemical evolution from the prestellar phase to the formation of the disk, and to determine the impact that the chemical composition of the cold and dense core has on the final composition of the disk. We performed 3D nonideal magneto-hydrodynamic (MHD) simulations of a dense core collapse using the adaptive-mesh-refinement RAMSES code. For each particle ending in the young rotationally supported disk, we ran chemical simulations with the three-phase gas-grain chemistry code Nautilus. Two different sets of initial abundances, which are characteristic of cold cores, were considered. The final distributions of the abundances of common species were compared to each other, as well as with the initial abundances of the cold core. We find that the spatial distributions of molecules reflect their sensitivity to the temperature distribution. The main carriers of the chemical elements in the disk are usually the same as the ones in the cold core, except for the S-bearing species, where HS is replaced by H${}_2$S${}_3$, and the P-bearing species, where atomic P leads to the formation of PO, PN, HCP, and CP. However, the abundances of less abundant species change over time. This is especially the case for "large" complex organic molecules (COMs) such as CH${}_3$CHO, CH${}_3$NH${}_2$, CH${}_3$OCH${}_3$, and HCOOCH${}_3$ which see their abundances significantly increase during the collapse. These COMs often present similar abundances in the disk despite significantly different abundances in the cold core. In contrast, the abundances of many radicals decrease with time. A significant number of species still show the same abundances in the cold core and the disk, which indicates efficient formation of these molecules in the cold core. This includes H${}_2$O, H${}_2$CO, HNCO, and "small" COMs such as CH${}_3$OH, CH${}_3$CN, and NH${}_2$CHO.

Accepted in Astronomy & Astrophysics, 44 pages, 36 figures

References in corpus (29)

• Non-thermal desorption from interstellar dust grains via exothermic surface reactions
• A High Order Godunov Scheme with Constrained Transport and Adaptive Mesh Refinement for Astrophysical MHD
• The ALMA Protostellar Interferometric Line Survey (PILS): First results from an unbiased submillimeter wavelength line survey of the Class 0 protostellar binary IRAS 16293-2422 with ALMA
• The 2014 KIDA network for interstellar chemistry
• The cometary composition of a protoplanetary disk as revealed by complex cyanides
• The origin of complex organic molecules in prestellar cores
• Molecular Evolution and Star Formation: From Prestellar Cores to Protostellar Cores
• Binding energies: new values and impact on the efficiency of chemical desorption
• The chemical history of molecules in circumstellar disks. I. Ices
• An interferometric study of the low-mass protostar IRAS 16293-2422: small scale organic chemistry
• Kinematic Dynamos using Constrained Transport with High Order Godunov Schemes and Adaptive Mesh Refinement
• Magnetically self-regulated formation of early protoplanetary discs
• Cometary ices in forming protoplanetary disc midplanes
• The interstellar chemistry of C3H and C3H2 isomers
• Methanol Along the Path from Envelope to Protoplanetary Disc
• Gas composition of main volatile elements in protoplanetary discs and its implication for planet formation
• Detection of glycolaldehyde towards the solar-type protostar NGC1333 IRAS2A
• A new look at sulphur chemistry in hot cores and corinos
• Water delivery from cores to disks: deuteration as a probe of the prestellar inheritance of H2O
• Orbital and mass constraints of the young binary system IRAS 16293-2422 A
• An unbiased ALMA spectral survey of the LkCa 15 and MWC 480 protoplanetary disks
• The ALMA-PILS survey: First detection of nitrous acid (HONO) in the interstellar medium
• The ALMA-PILS survey: First detection of the unsaturated 3-carbon molecules Propenal (C${}_2$H${}_3$CHO) and Propylene (C${}_3$H${}_6$) towards IRAS 16293$-$2422 B
• Protostellar collapse: A comparison between SPH and AMR calculations
• Chemistry in a forming protoplanetary disk: main accretion phase
• Modeling the chemical evolution of a collapsing prestellar core in two spatial dimensions
• Importance of the H2 abundance in protoplanetary disk ices for the molecular layer chemical composition
• A fast tree-based method for estimating column densities in Adaptive Mesh Refinement codes Influence of UV radiation field on the structure of molecular clouds
• Physicochemical models: source-tailored or generic?

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• Chemical post-processing of magneto-hydrodynamical simulations of star-forming regions: robustness and pitfalls
• Dynamics of dust grains in turbulent molecular clouds. Conditions for decoupling and limits of different numerical implementations
• The initial magnetic criticality of prestellar cores
• Chemical inventory of the envelope of the Class I protostar L1551 IRS 5
• Gas phase Elemental abundances in Molecular cloudS (GEMS). X. Observational effects of turbulence on the chemistry of molecular clouds