Time-distance helioseismology: Sensitivity of f-mode travel times to flows

TL;DR

This paper develops a theoretical framework for understanding how horizontal flows in the Sun affect f-mode helioseismic travel times, providing sensitivity kernels that aid in interpreting solar flow measurements.

Contribution

It introduces two-dimensional Fréchet kernels for f-mode travel-time sensitivity to local flows, enhancing interpretation of helioseismic data.

Findings

Travel-time shifts are linear for flows under 250 m/s.

Third-order perturbation theory is needed for stronger flows.

The kernels show that flow effects depend on damping and observation direction.

Abstract

Time-distance helioseismology has shown that f-mode travel times contain information about horizontal flows in the Sun. The purpose of this study is to provide a simple interpretation of these travel times. We study the interaction of surface-gravity waves with horizontal flows in an incompressible, plane-parallel solar atmosphere. We show that for uniform flows less than roughly 250 m s$^{-1}$, the travel-time shifts are linear in the flow amplitude. For stronger flows, perturbation theory up to third order is needed to model waveforms. The case of small-amplitude spatially-varying flows is treated using the first-order Born approximation. We derive two-dimensional Fr\'{e}chet kernels that give the sensitivity of travel-time shifts to local flows. We show that the effect of flows on travel times depends on wave damping and on the direction from which the observations are made. The main physical effect is the advection of the waves by the flow rather than the advection of wave sources or the effect of flows on wave damping. We compare the two-dimensional sensitivity kernels with simplified three-dimensional kernels that only account for wave advection and assume a vertical line of sight. We find that the three-dimensional f-mode kernels approximately separate in the horizontal and vertical coordinates, with the horizontal variations given by the simplified two-dimensional kernels. This consistency between quite different models gives us confidence in the usefulness of these kernels for interpreting quiet-Sun observations.