Abstract
After core helium burning in low and intermediate-mass stars, starts the AGB phase. In this phase, the s process takes place, which is believed to be at the origin of half of all elements heavier than iron. The role of rotation and magnetic fields on the AGB phase is still debated and uncertain. We have calculated stellar evolution models with MESA for stars with an initial mass of 1.5 and 3.0 solar masses. Our models include both rotation and the Taylor-Spruit (TS) dynamo. We show how these physical processes contribute to the total diffusion coefficient and how it will effect the transport of angular momentum and the s-process nucleosynthesis.Our preliminary results confirm previous results that inclusion of rotation and the TS dynamo, compared to inclusion of rotation alone, results in an improvement of the predicted rotational period of white dwarfs. Inclusion of the TS dynamo reduces the rotationally induced mixing. The impact on the s-process nucleosynthesis is underway and will be presented in a forthcoming publication.
Highlights
We have calculated stellar evolution models with MESA for stars with an initial mass of 1.5 and 3.0 solar masses. Our models include both rotation and the Taylor-Spruit (TS) dynamo. We show how these physical processes contribute to the total diffusion coefficient and how it will effect the transport of angular momentum and the s-process nucleosynthesis
AGB stars and white dwarfs After core helium burning is over an unstable phase of hydrogen shell burning and helium shell flash events starts [1]
Grid of models To check the effect of rotation and the TS-dynamo, we ran stellar evolution models with MESA for two different masses (1.5 M and 3.0 M ) and two metallicities (Z = 0.001 and Z = 0.02)
Summary
After core helium burning in low and intermediate-mass stars, starts the AGB phase. Our models include both rotation and the Taylor-Spruit (TS) dynamo. We show how these physical processes contribute to the total diffusion coefficient and how it will effect the transport of angular momentum and the s-process nucleosynthesis.
Sign-in/Register to view highlights & summary Sign-in/Register to access full text options 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
