The chemistry of protoplanetary fragments formed via gravitational instabilities

Abstract

In this paper, we model the chemical evolution of a 0.25 M${}_{\odot }$ protoplanetary disc surrounding a 1 M${}_{\odot }$ star that undergoes fragmentation due to self-gravity. We use Smoothed Particle Hydrodynamics including a radiative transfer scheme, along with time-dependent chemical evolution code to follow the composition of the disc and resulting fragments over approximately 4000 yrs. 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. H${}_2$O, H${}_2$S, HNO, N${}_2$, NH${}_3$, OCS, SO), species that are abundant in the spiral shocks within the disc (e.g. CO, CH${}_4$, CN, CS, H${}_2$CO), and species which 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.

17 pages, 7 figures, accepted for publication in MNRAS

References in corpus (19)

• Direct Imaging of Multiple Planets Orbiting the Star HR 8799
• SPLASH: An interactive visualisation tool for Smoothed Particle Hydrodynamics simulations
• Spiral Density Waves in a Young Protoplanetary Disk
• Towards Chemical Constraints on Hot Jupiter Migration
• A Triple Protostar System Formed via Fragmentation of a Gravitationally Unstable Disk
• Chemical enrichment of giant planets and discs due to pebble drift
• Imaging the water-snow line during a protostellar outburst
• Setting the volatile composition of (exo)planet-building material. Does chemical evolution in disk midplanes matter?
• Fragmentation of gravitationally unstable gaseous protoplanetary disks with radiative transfer
• Radiative transfer and the energy equation in SPH simulations of star formation
• A Sub-arcsecond Survey Toward Class 0 Protostars in Perseus: Searching for Signatures of Protostellar Disks
• Introducing a Hybrid Method of Radiative Transfer for Smoothed Particle Hydrodynamics
• Planetesimal Capture in the Disk Instability Model
• Identifying and Analysing Protostellar Disc Fragments in Smoothed Particle Hydrodynamics Simulations
• How to Detect the Signatures of Self-Gravitating Circumstellar Discs with the Atacama Large Millimetre/sub-millimetre Array
• Grand challenges in protoplanetary disc modelling
• The Dynamical Fate of Self-Gravitating Disc Fragments After Tidal Downsizing
• Effects of disc midplane evolution on CO snowline location
• Gravitational instabilities in a protosolar-like disc II: continuum emission and mass estimates

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