# Angular momentum transport by magnetic fields in main sequence stars with Gamma Doradus pulsators

**Authors:** F. D. Moyano, P. Eggenberger, S. J. A. J. Salmon, J. S. G. Mombarg, S. Ekström  
**arXiv:** [2304.00674](https://arxiv.org/abs/2304.00674)  
**Date:** 2023-04-03  
**Summary page:** https://www.summarizepaper.com/en/paper/2304.00674v1/

## Key points

- Investigates internal angular momentum (AM) transport in main sequence stars, particularly Gamma Doradus ($\gamma$ Dor) stars.
- Tests whether models of rotating stars with internal magnetic fields can reproduce their rotational properties.
- Compiles observational constraints for $\gamma$ Dor stars from the literature, including core rotation rates and projected rotational velocities from spectroscopy, as well as fundamental parameters such as effective temperature and metallicity.
- Computes rotating models with the Geneva stellar evolution code taking into account meridional circulation and shear instability.
- Creates models with internal magnetic fields using a general formalism for transport by the Tayler-Spruit dynamo.
- Comparing these models to observational constraints reveals that:
- Stellar models with purely hydrodynamical processes are in disagreement with the data
- Models with internal magnetic fields can reproduce both core and surface constraints simultaneously
- Result is consistent with previous studies on subgiant and red giant stars, indicating that angular momentum transport in radiative regions of $\gamma$ Dor stars is highly efficient and in good agreement with predictions of models with internal magnetic fields.
- Includes sections describing input physics used in their models, comparisons made between model predictions and observations, uncertainties present in their conclusions, additional evidence supporting their analysis, discussion of results in context of more evolved stars, and finally a summary and conclusion section.
- Provides valuable insights into our understanding of AM transport processes in main sequence stars.

## Summary

This paper investigates the internal angular momentum (AM) transport in main sequence stars, particularly Gamma Doradus ($\gamma$ Dor) stars. It tests whether models of rotating stars with internal magnetic fields can reproduce their rotational properties. The authors compile observational constraints for $\gamma$ Dor stars from the literature, including core rotation rates and projected rotational velocities from spectroscopy, as well as fundamental parameters such as effective temperature and metallicity. They then compute rotating models with the Geneva stellar evolution code taking into account meridional circulation and shear instability. Additionally, they create models with internal magnetic fields using a general formalism for transport by the Tayler-Spruit dynamo. Comparing these models to observational constraints reveals that stellar models with purely hydrodynamical processes are in disagreement with the data whereas those with internal magnetic fields can reproduce both core and surface constraints simultaneously. This result is consistent with previous studies on subgiant and red giant stars, indicating that angular momentum transport in radiative regions of $\gamma$ Dor stars is highly efficient and in good agreement with predictions of models with internal magnetic fields. The paper includes sections describing input physics used in their models, comparisons made between model predictions and observations, uncertainties present in their conclusions, additional evidence supporting their analysis, discussion of results in context of more evolved stars, and finally a summary and conclusion section. Overall, this study provides valuable insights into our understanding of AM transport processes in main sequence stars.