Prospects for the Detection of the Deep Solar Meridional Circulation

Abstract

We perform helioseismic holography to assess the noise in p-mode travel-time shifts which would form the basis of inferences of large-scale flows throughout the solar convection zone. We also derive the expected travel times from a parameterized return (equatorward) flow component of the meridional circulation at the base of the convection zone from forward models under the assumption of the ray and Born approximations. From estimates of the signal-to-noise ratio for measurements focused near the base of the convection zone, we conclude that the helioseismic detection of the deep meridional flow including the return component may not be possible using data spanning an interval less than a solar cycle.

References in corpus (3)

• Subsurface Meridional Circulation in the Active Belts
• Linear Sensitivity of Helioseismic Travel Times to Local Flows
• Meridional Circulation and Global Solar Oscillations

Cited by in corpus (6)

• Helioseismology of Pre-Emerging Active Regions I: Overview, Data, and Target Selection Criteria
• Helioseismology with Solar Orbiter
• Full Waveform Inversion of Solar Interior Flows
• Helioseismic Modeling of Background Flows
• Quantitative passive imaging by iterative holography: The example of helioseismic holography
• Constraining Global Solar Models through Helioseismic Analysis