The dynamics of the radiative zone of the Sun

TL;DR

This paper investigates the Sun's radiative zone dynamics by modeling rotation histories, magnetic fields, and mass loss, comparing results with helioseismic data to understand their impact on solar structure.

Contribution

It introduces models with varied rotation histories and assesses their effects on the Sun's radiative zone, incorporating magnetic fields and mass loss to improve understanding.

Findings

Rotation history significantly affects sound speed profiles.

Magnetic fields influence the internal rotation and structure.

Mass loss impacts the evolution of the radiative zone.

Abstract

Helioseismology puts strong constraints on the internal sound speed and on the rotation profile in the radiative zone. Young stars of solar type are more active and faster rotators than the Sun. So we begin to build models which include different rotation histories and compare the results with all the solar observations. The profiles of the rotation we get have interesting consequence for the introduction of magnetic field in the radiative zone. We discuss also the impact of mass loss deduced from measured flux of young stars. We deduce from these comparisons some quantitative effect of the dynamical processes (rotation, magnetic field and mass loss) of these early stages on the present sound speed and density. We show finally how we can improve our present knowledge of the radiative zone with PICARD and GOLFNG.