The Impact of Carbon Enhancement on Extra Mixing in Metal-Poor Stars

TL;DR

This study investigates how carbon enhancement affects internal mixing processes in metal-poor stars, challenging existing models of thermohaline mixing and revealing suppressed extra mixing in CEMP giants.

Contribution

It provides new observational evidence that thermohaline mixing is ineffective in CEMP stars and shows that canonical extra mixing is suppressed in these stars compared to similar metallicity stars.

Findings

Dilution of CN in giant CEMP stars indicates ineffective thermohaline mixing.

Canonical extra mixing is suppressed in CEMP giants.

Data suggest slower thermohaline mixing on the main sequence.

Abstract

We critically examine the constraints imposed by carbon-enhanced metal-poor (CEMP) stars on the mixing mechanisms that operate in red giants. CEMP stars are created when the surface layers of a metal-poor dwarf are enriched with He-burning products via mass transfer from an evolved donor. The difference between main sequence (MS) and red giant CEMP abundances can be used as a diagnostic of the timescale for the mixing of the processed material into stellar interiors on the MS. Abundance trends with luminosity among red giant CEMP stars test theories of canonical extra mixing for low mass giants with a high bulk metallicity. We find a significant dilution in CN enrichment in giant CEMP stars relative to their MS precursors, and take this as evidence that thermohaline mixing induced by mean molecular weight inversions is ineffective in CEMP stars. This contradicts models that rely on efficient thermohaline mixing induced by small mu gradients in red giants, because such models would predict that MS CEMP stars with large mu inversions would be homogenized on a very short timescale. The data do not rule out slower MS thermohaline mixing comparable to previously published estimates. We also find that canonical extra mixing is strongly suppressed in CEMP giants relative to stars with the same iron abundance. A likely cause is the shift in the location of non-equilibrium CN processing relative to the steep mu gradient in the hydrogen burning shell, which also occurs in solar metallicity RGB stars. Implications for the mass accreted by CEMP stars and the mechanism for canonical extra mixing are discussed.