3He-Driven Mixing in Low-Mass Red Giants: Convective Instability in Radiative and Adiabatic Limits

TL;DR

This paper investigates the stability of 3He-driven mixing in low-mass red giants, identifying thermohaline convection as a key process and discussing obstacles to its effectiveness and observational evidence of extra mixing.

Contribution

It analyzes the physical mechanisms of 3He-induced mixing, identifies conditions for thermohaline convection, and discusses challenges to its role in stellar mixing processes.

Findings

Two unstable modes identified: a rapid adiabatic and a slow radiative (thermohaline)

Thermohaline convection requires finger-like structures with l/d > 10

Rotation-induced turbulence may suppress thermohaline mixing

Abstract

We examine the stability and observational consequences of mixing induced by 3He burning in the envelopes of first ascent red giants. We demonstrate that there are two unstable modes: a rapid, nearly adiabatic mode that we cannot identify with an underlying physical mechanism, and a slow, nearly radiative mode that can be identified with thermohaline convection. We present observational constraints that make the operation of the rapid mode unlikely to occur in real stars. Thermohaline convection turns out to be fast enough only if fluid elements have finger-like structures with a length to diameter ratio l/d > 10. We identify some potentially serious obstacles for thermohaline convection as the predominant mixing mechanism for giants. We show that rotation-induced horizontal turbulent diffusion may suppress the 3He-driven thermohaline convection. Another potentially serious problem for it is to explain observational evidence of enhanced extra mixing. The 3He exhaustion in stars approaching the red giant branch (RGB) tip should make the 3He mixing inefficient on the asymptotic giant branch (AGB). In spite of this, there are observational data indicating the presence of extra mixing in low-mass AGB stars similar to that operating on the RGB. Overmixing may also occur in carbon-enhanced metal-poor stars.