Under certain conditions, the cores of stars contract. When this happens, they start to spin faster than the external layers of the star. However, the study of oscillations in stars, asteroseismology, has uncovered an astonishing phenomenon: the cores of such stars actually rotate more slowly than calculations predict. Why is this so? Three French scientists, from CNRS, INRIA and ENS-PSL have studied this question and report their findings in an article published in Science  on January 20, 2023. Their numerical simulations, which model plasma flow in the deep layers of a star, have shown that the slowing down of the core can be produced by an internal magnetic field. More specifically, plasma flow can amplify a magnetic field to the point where it generates strong turbulent motions. Such turbulence may further amplify the magnetic field until it causes the star’s core to spin down. The results obtained with the research team’s simulations are also in agreement with asteroseismological observations of many stars. In addition, the simulations show that the magnetic field would be hidden by the outer layers of the star, which explains why no magnetic field of this kind has yet been measured with current techniques.

Simulation showing the intense magnetic field generated inside the radiative layer of a star (white lines). The magnetic field generates strong turbulence in the plasma (blue lines) in the internal regions of the star, which spin down. Since the magnetic field is toroidal (torus- or doughnut-shaped) and located deep in the radiative region, it is hidden from the exterior.
© Christophe Gissinger




Author affiliation:
Laboratoire de physique de L’École normale supérieure (LPENS, ENS Paris/CNRS/Sorbonne Université/Université de Paris)

Corresponding author: Christophe Gissinger
Communication contact: L’équipe de communication