The chemistry of protoplanetary fragments formed via gravitational instabilities

Abstract In this paper, we model the chemical evolution of a 0.25 M⊙ protoplanetary disc surrounding a 1 M⊙ star that undergoes fragmentation due to self-gravity. We use smoothed particle hydrodynamics including a radiative transfer scheme, along with a time-dependent chemical evolution code to foll...

Full description

Saved in:
Bibliographic Details
Published in:Monthly notices of the Royal Astronomical Society 2017-11, Vol.472 (1), p.189-204
Main Authors: Ilee, J. D., Forgan, D. H., Evans, M. G., Hall, C., Booth, R., Clarke, C. J., Rice, W. K. M., Boley, A. C., Caselli, P., Hartquist, T. W., Rawlings, J. M. C.
Format: Article
Language:English
Subjects:
Ammonia
Atmospheric composition
Atmospheric models
Chemical composition
Chemical evolution
Computational fluid dynamics
Fluid flow
Fragmentation
Fragments
Gravitation
Gravitational instability
Hydrodynamics
Organic chemistry
Planetary composition
Radiative transfer
Smooth particle hydrodynamics
Time dependence
Volatile compounds
Citations: Items that this one cites
Items that cite this one
Online Access:Request full text
Tags: Add Tag
No Tags, Be the first to tag this record!
Description
Summary:Abstract In this paper, we model the chemical evolution of a 0.25 M⊙ protoplanetary disc surrounding a 1 M⊙ star that undergoes fragmentation due to self-gravity. We use smoothed particle hydrodynamics including a radiative transfer scheme, along with a time-dependent chemical evolution code to follow the composition of the disc and resulting fragments over approximately 4000 yr. Initially, four quasi-stable fragments are formed, of which two are eventually disrupted by tidal torques in the disc. From the results of our chemical modelling, we identify species that are abundant in the fragments (e.g. H2O, H2S, HNO, N2, NH3, OCS, SO), species that are abundant in the spiral shocks within the disc (e.g. CO, CH4, CN, CS, H2CO) and species that are abundant in the circumfragmentary material (e.g. HCO+). Our models suggest that in some fragments it is plausible for grains to sediment to the core before releasing their volatiles into the planetary envelope, leading to changes in, e.g., the C/O ratio of the gas and ice components. We would therefore predict that the atmospheric composition of planets generated by gravitational instability should not necessarily follow the bulk chemical composition of the local disc material.
ISSN:0035-8711
1365-2966
DOI:10.1093/mnras/stx1966