Li-rich and super Li-rich giants produced by element diffusion^⋆

¹ School of Physical Science and Technology, Xinjiang University, Urumqi 830046, PR China
e-mail: guolianglv@xao.ac.cn
² Center for Theoretical Physics, Xinjiang University, Urumqi 830046, PR China
³ College of Mechanical and Electronic Engineering, Tarim University, Alar 843300, PR China
⁴ CAS Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, PR China
⁵ School of Astronomy and Space Science, University of Chinese Academy of Sciences, Beijing 100101, PR China

Received: 26 April 2022
Accepted: 17 October 2022

Abstract

Context. About 0.2−2% of giant stars are Li rich, that is to say their lithium abundance (A(Li)) is higher than 1.5 dex. Nearly 6% of these Li-rich giant stars are super Li rich, with an A(Li) exceeding 3.2 dex. Meanwhile, the formation mechanism of these Li-rich and super Li-rich giants is still under debate.

Aims. Considering the compact He core of red giants, attention is paid to the effect of element diffusion on A(Li). In particular, when the He-core flash occurs, element diffusion makes the thermohaline mixing zone extend inward and connect to the inner convection region of stars. Then, a large amount of ⁷Be produced by the He flash can be transferred to the stellar surface, finally turning into ⁷Li. Thus, the goal of this work is to propose the mechanism of A(Li) enrichment and achieve consistency between the theoretical and observation data.

Methods. Using the Modules for Experiments in Stellar Astrophysics (MESA) stellar evolution code, we simulated the evolution of low-mass stars, considering the effects of element diffusion on the Li abundances. The timescale ratio of Li-rich giants to normal giants was estimated using the population synthesis method. Then we obtained the theoretical value of A(Li) and made a comparison with observations.

Results. Considering the influence of element diffusion in the model results in the increase of the lithium abundance up to about 1.8 dex, which can reveal Li-rich giants. Simultaneously, introducing high constant diffusive mixing coefficients (D_mix) with the values from 10¹¹ to 10¹⁵ cm² s⁻¹ in the model allows the A(Li) to increase from 2.4 to 4.5 dex, which can explain most of the Li-rich and super Li-rich giant stars. The population synthesis method reveals that the amount of Li-rich giants is about 0.2−2% of all giants, which is consistent with observation estimated levels.

Conclusions. In our models the element diffusion, mainly triggered by the gravity field, changes the mean molecular weight at the junction zone between the stellar envelope and the He core, which makes the thermohaline mixing region expand to the inner convection region of stars. A transport channel, efficiently transporting ⁷Be in the hydrogen-burning region of the star to the convective envelope where ⁷Be decays into ⁷Li, is formed. Combining high constant diffusive mixing coefficients, the transport channel can explain the origin of Li-rich and super Li-rich giants, even the most super Li-rich giants.