# The partial ionisation zone of heavy elements in F-stars: a study on how it correlates with rotation

## TL;DR

This study explores how the partial ionisation zones of heavy elements in F-stars relate to their internal structure and rotation, revealing potential links between magnetic activity, convection, and ionisation regions.

## Contribution

It provides new insights into the correlation between the location of ionisation zones and rotational regimes in F-stars, highlighting their role in stellar magnetic dynamics.

## Key findings

- Two distinct rotational regimes linked to ionisation zones
- The relative position of ionisation regions distinguishes rotation types
- Magnetic field properties may be connected to ionisation and convection

## Abstract

We study the relation between the internal structures of 10 benchmark main-sequence F-stars and their rotational properties. Stellar rotation of main-sequence F-type stars can be characterised by two distinct rotational regimes. Early-type F-stars are usually rapid rotators with periods typically below 10 days, whereas later-type F-stars have longer rotation periods. Specifically, and since the two rotational regimes are tightly connected to the effective temperatures of the stars, we investigate in detail the characteristics of the partial ionisation zones in the outer convective envelopes of these stars, which in turn, depend on the internal temperature profiles. Our study shows that the two rotational regimes might be distinguished by the relative locations of the partial ionisation region of heavy elements and the base of the convective zone. Since in all these stars is expected a dynamo-driven magnetic field where the shear layer between convective and radiative zones (tachocline) plays an important role, this result suggests that the magnetic field may be related to the combined properties of convection and ionisation.