The galactic chemical evolution of carbon: Implications for stellar nucleosynthesis

TL;DR

This study uses Galactic chemical evolution models and APOGEE data to determine the relative contributions of supernovae and AGB stars to carbon production in the Milky Way, finding CCSN yields increase with metallicity and AGB stars contribute 10-40%.

Contribution

It provides new constraints on the sources of galactic carbon, especially quantifying AGB stars' contribution and the metallicity dependence of supernova yields.

Findings

AGB stars contribute 10-40% of carbon at solar metallicity.

CCSN yields likely increase with metallicity to match observations.

Discrepancies suggest possible revisions in stellar evolution models.

Abstract

Carbon (C) is thought to be produced by both core collapse supernovae (CCSN) and asymptotic giant branch (AGB) stars, but the relative contributions of these two sources are uncertain. We investigate the astrophysical origin of C using models of Galactic chemical evolution (GCE) appropriate for the Milky Way disk. We benchmark our results against APOGEE subgiant abundances. The trend between [C/Mg] and [Mg/H] is set by the total C yield as a function of metallicity. Observations indicate a gently rising [C/Mg] with [Mg/H], but AGB C production is predicted to decline with metallicity. Our sample therefore favours a scenario in which CCSN yields rise with metallicity to offset declining AGB C yields and drive a subtle increase in [C/Mg] with [Mg/H]. This result is consistent with massive star nucleosynthesis models incorporating rotation. The [C/Mg]-[Mg/Fe] trend is sensitive to delayed enrichment and therefore constrains the amount of AGB C production. Given the slope of this relation, we find that AGB stars likely account for 10-40 per cent of C at solar metallicity. Artificially shifting the AGB C yields towards lower mass stars with longer lifetimes also improves agreement with the observed [C/Mg]-[Mg/Fe] trend, possibly indicating a discrepancy with stellar evolution predictions or our assumed Fe production rate.