The effects of the carbon-to-oxygen ratio on the condensate compositions around Solar-like stars

TL;DR

This study uses a dust condensation model to explore how varying stellar C/O ratios influence the composition of solids in protoplanetary disks around Solar-like stars, revealing distinct system types and significant carbon condensation effects.

Contribution

It provides a detailed analysis of how initial stellar C/O ratios determine the dominant condensed species and system types, highlighting the importance of C/O variations up to 1.

Findings

Solar system corresponds to low C/O ratio systems (0.52-0.6)

Intermediate systems show decreasing silicates and increasing carbides

Carbon can constitute over 80% of condensed mass at certain radii

Abstract

The initial stellar carbon-to-oxygen (C/O) ratio can have a large impact on the resulting condensed species present in the protoplanetary disk and, hence, the composition of the bodies and planets that form. The observed C/O ratios of stars can vary from 0.1-2. We use a sequential dust condensation model to examine the impact of the C/O ratio on the composition of solids around a Solar-like star. We utilize this model in a focused examination of the impact of varying the initial stellar C/O ratio to isolate the effects of the C/O ratio in the context of Solar-like stars. We describe three different system types in our findings. The Solar system falls into the silicate-dominant, low C/O ratio systems which end at a stellar C/O ratio somewhere between 0.52 and 0.6. At C/O ratios between about 0.6 and 0.9, we have intermediate systems. Intermediate systems show a decrease in silicates while carbides begin to become significant. Carbide-dominant systems begin around a C/O ratio of 0.9. Carbide-dominant systems exhibit high carbide surface densities at inner radii with comparable levels of carbides and silicates at outer radii. Our models show that changes between C/O=0.8 and C/O=1 are more significant than previous studies, that carbon can exceed 80% of the condensed mass, and that carbon condensation can be significant at radii up to 6 AU.