High-resolution mapping of flows in the solar interior: Fully consistent OLA inversion of helioseismic travel times

TL;DR

This paper develops a fully consistent 3D inversion method using finite-frequency sensitivity kernels and OLA to map solar interior flows with high resolution, minimizing cross-talk and accurately estimating errors.

Contribution

It introduces a novel 2+1D OLA inversion scheme with full noise covariance utilization for helioseismic travel-time data, improving flow mapping accuracy.

Findings

Achieved 7-10 Mm resolution flow maps in the quiet Sun.

Inversion results show very small cross-talk among flow components.

Flow maps correlate with Doppler data at 0.9.

Abstract

To recover the flow information encoded in travel-time data of time-distance helioseismology, accurate forward modeling and a robust inversion of the travel times are required. We accomplish this using three-dimensional finite-frequency travel-time sensitivity kernels for flows along with a 2+1 dimensional (2+1D) optimally localized averaging (OLA) inversion scheme. Travel times are measured by ridge filtering MDI full-disk Doppler data and the corresponding Born sensitivity kernels are computed for these particular travel times. We also utilize the full noise covariance properties of the travel times which allow us to accurately estimate the errors for all inversions. The whole procedure is thus fully consistent. Due to ridge filtering, the kernel functions separate in the horizontal and vertical directions, motivating our choice of a 2+1D inversion implementation. The inversion procedure also minimizes cross-talk effects among the three flow components, and the averaging kernels resulting from the inversion show very small amounts of cross-talk. We obtain three-dimensional maps of vector solar flows in the quiet Sun at spatial resolutions of 7-10 Mm using generally 24 h of data. For all of the flow maps we provide averaging kernels and the noise estimates. We present examples to test the inferred flows, such as a comparison with Doppler data, in which we find a correlation of 0.9. We also present results for quiet-Sun supergranular flows at different depths in the upper convection zone.