Differential rotation and radiative equilibrium in the Sun: is the tachocline spreading?

TL;DR

This paper investigates whether the Sun's tachocline can maintain radiative equilibrium without spreading, showing that minimal deviations from uniform rotation suffice and that radiative equilibrium is plausible in this region.

Contribution

It derives a differential equation for the Sun's rotation profile under radiative equilibrium and demonstrates solutions that match helioseismic data, challenging previous views on tachocline spreading.

Findings

Radiative equilibrium solutions closely match helioseismic rotation profiles.

Minimal baroclinic deviations are needed to sustain radiative equilibrium.

The tachocline spreading issue may be less problematic than previously believed.

Abstract

It is well known that the combination of barotropic rotation and radiative equilibrium are mutually incompatible in stars. The Sun's internal rotation is far from barotropic, however, which allows at least the theoretical possibility that the Sun's thermal balance is one of radiative equilibrium in the region of the tachocline near the outer boundary of the radiative zone. We show here that (i) the constraint of radiative equilibrium leads to a straightforward ordinary differential equation for the Sun's rotation profile, and (ii) solutions of this equation can be found that, to within current levels of accuracy, closely resemble the rotation profile deduced from helioseismology. More generally, we calculate how large a baroclinic deviation from uniform rotation is required to maintain radiative equilibrium without meridional circulation throughout the bulk of the radiative zone. Very little deviation is required, well below detectability. The feasibility of radiative equilibrium for the tachocline suggests that the issue of a spreading boundary layer may be less severe than previously thought.