Helioseismology of sunspots: how sensitive are travel times to the Wilson depression and to the subsurface magnetic field?

Abstract

In order to assess the ability of helioseismology to probe the subsurface structure and magnetic field of sunspots, we need to determine how helioseismic travel times depend on perturbations to sunspot models. Here we numerically simulate the propagation of f, p1, and p2 wave packets through magnetic sunspot models. Among the models we considered, a ~50 km change in the height of the Wilson depression and a change in the subsurface magnetic field geometry can both be detected above the observational noise level. We also find that the travel-time shifts due to changes in a sunspot model must be modeled by computing the effects of changing the reference sunspot model, and not by computing the effects of changing the subsurface structure in the quiet-Sun model. For p1 modes the latter is wrong by a factor of four. In conclusion, numerical modeling of MHD wave propagation is an essential tool for the interpretation of the effects of sunspots on seismic waveforms.

5 pages, 3 figures: submitted to A&A

References in corpus (5)

• Helioseismology of Sunspots: Confronting Observations with Three-Dimensional MHD Simulations of Wave Propagation
• SLiM: a code for the simulation of wave propagation through an inhomogeneous, magnetised solar atmosphere
• Scattering of acoustic waves by a magnetic cylinder
• Physical Properties of Wave Motion in Inclined Magnetic Fields Within Sunspot Penumbrae
• Seismic probes of solar interior magnetic structure

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