English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

Stellar magnetism plays an important role in stellar evolution theory.Approximatively 10% of observed main sequence (MS) and pre-main-sequence (PMS)radiative stars exhibit surface magnetic fields above the detection limit,raising the question of their origin. These stars host outer radiativeenvelopes, which are stably stratified. Therefore, they are assumed to bemotionless in standard models of stellar structure and evolution. We focus onrapidly rotating, radiative stars which may be prone to the tidal instability,due to an orbital companion. Using direct numerical simulations in a sphere, westudy the interplay between a stable stratification and the tidal instability,and assess its dynamo capability. We show that the tidal instability istriggered regardless of the strength of the stratification(Brunt-V{\"a}is{\"a}l{\"a} frequency). Furthermore, the tidal instability canlead to both mixing and self-induced magnetic fields in stably stratifiedlayers (provided that the Brunt-V{\"a}is{\"a}l{\"a} frequency does not exceedthe stellar spin rate in the simulations too much). The application to starssuggests that the resulting magnetic fields could be observable at the stellarsurfaces. Indeed, we expect magnetic field strengths up to severalGauss.Consequently, tidally driven dynamos should be considered as a(complementary) dynamo mechanism, possibly operating in radiative MS and PMSstars hosting orbital companions. In particular, tidally driven dynamos mayexplain the observed magnetism of tidally deformed and rapidly rotatingVega-like stars.

Magnetic fields driven by tidal mixing in radiative stars