Estimating the deep solar meridional circulation using magnetic observations and a dynamo model: a variational approach

TL;DR

This paper introduces a variational data assimilation method using magnetic observations and a solar dynamo model to accurately estimate the Sun's large-scale meridional circulation, enhancing understanding and prediction of solar activity.

Contribution

It presents a novel variational approach with adjoint modeling to infer the Sun's meridional flow from magnetic data, validated through synthetic experiments.

Findings

Method recovers true meridional flow within 1% in synthetic tests.

Robustness across different flow configurations and observational setups.

Potential to improve solar activity prediction and understanding.

Abstract

We show how magnetic observations of the Sun can be used in conjunction with an axisymmetric flux-transport solar dynamo model in order to estimate the large-scale meridional circulation throughout the convection zone. Our innovative approach rests on variational data assimilation, whereby the distance between predictions and observations (measured by an objective function) is iteratively minimized by means of an optimization algorithm seeking the meridional flow which best accounts for the data. The minimization is performed using a quasi-Newton technique, which requires the knowledge of the sensitivity of the objective function to the meridional flow. That sensitivity is efficiently computed via the integration of the adjoint flux-transport dynamo model. Closed-loop (also known as twin) experiments using synthetic data demonstrate the validity and accuracy of this technique, for a variety of meridional flow configurations, ranging from unicellular and equatorially symmetric to multicellular and equatorially asymmetric. In this well-controlled synthetic context, we perform a systematic study of the behavior of our variational approach under different observational configurations, by varying their spatial density, temporal density, noise level, as well as the width of the assimilation window. We find that the method is remarkably robust, leading in most cases to a recovery of the true meridional flow to within better than 1%. These encouraging results are a first step towards using this technique to i) better constrain the physical processes occurring inside the Sun and ii) better predict solar activity on decadal time scales.