Gyroscopic Pumping in the Solar Near-Surface Shear Layer

TL;DR

This paper investigates the dynamics of the solar Near-Surface Shear Layer using helioseismic data, revealing the role of turbulent angular momentum transport and force balance in shaping the layer's structure.

Contribution

It demonstrates that turbulent stresses, not surface convection alone, maintain the NSSL's shear profile and identifies the transition from baroclinic to turbulent stresses at its base.

Findings

Turbulent angular momentum transport is non-diffusive and inward-directed.

Maintaining the NSSL requires 2-4% of solar luminosity.

The spin-down time scale of the NSSL is approximately 600 days.

Abstract

We use global and local helioseismic inversions to explore the prevailing dynamical balances in the solar Near-Surface Shear Layer (NSSL). The differential rotation and meridional circulation are intimately linked, with a common origin in the turbulent stresses of the upper solar convection zone. The existence and structure of the NSSL cannot be attributed to the conservation of angular momentum by solar surface convection, as is often supposed. Rather, the turbulent angular momentum transport accounts for the poleward meridional flow while the often overlooked meridional force balance maintains the mid-latitude rotational shear. We suggest that the base of the NSSL is marked by a transition from baroclinic to turbulent stresses in the meridional plane which suppress Coriolis-induced circulations that would otherwise establish a cylindrical rotation profile. The turbulent angular momentum transport must be non-diffusive and directed radially inward. Inferred mean flows are consistent with the idea that turbulent convection tends to mix angular momentum but only if the mixing efficiency is inhomogeneous and/or anisotropic. The latitudinal and longitudinal components of the estimated turbulent transport are comparable in amplitude and about an order of magnitude larger than the vertical component. We estimate that it requires 2--4% of the solar luminosity to maintain the solar NSSL against the inertia of the mean flow. Most of this energy is associated with the turbulent transport of angular momentum out of the layer, with a spin-down time scale of $\sim$ 600 days. We also address implications of these results for numerical modeling of the NSSL.