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/

Zendy Plus

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

Zendy Tools

Zendy Open

One of the major discoveries of asteroseismology is the signature of a strongextraction of angular momentum (AM) in the radiative zones of stars across theentire Hertzsprung-Russell diagram, resulting in weak core-to-surface rotationcontrasts. Despite all efforts, a consistent AM transport theory, whichreproduces both the internal rotation and mixing probed thanks to theseismology of stars, remains one of the major open problems in modern stellarastrophysics. A possible key ingredient to figure out this puzzle is magneticfield with its various possible topologies. Among them, strong axisymmetrictoroidal fields, which are subject to the so-called Tayler MHD instability,could play a major role. They could trigger a dynamo action in radiative layerswhile the resulting magnetic torque allows an efficient transport of AM. But isit possible to detect signatures of these deep toroidal magnetic fields? Theonly way to answer this question is asteroseismology and the best laboratoriesof study are intermediate-mass and massive stars because of their externalradiative envelope. Since most of these are rapid rotators during theirmain-sequence, we have to study stellar pulsations propagating in stablystratified, rotating, and potentially strongly magnetised radiative zones. Forthat, we generalise the traditional approximation of rotation, which providesin its classic version a flexible treatment of the adiabatic propagation ofgravito-inertial modes, by taking simultaneously general axisymmetricdifferential rotation and toroidal magnetic fields into account. Using this newnon-perturbative formalism, we derive the asymptotic properties ofmagneto-gravito-inertial modes and we explore the different possible fieldconfigurations. We found that the magnetic effects should be detectable forequatorial fields using high-precision asteroseismic data.

Can we detect deep axisymmetric toroidal magnetic fields in stars?