Helioseismology of sunspots: how sensitive are travel times to the Wilson depression and to the subsurface magnetic field?
Abstract
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, p_{1}, and p_{2} 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 traveltime 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 quietSun model. For p_{1} modes, the latter is wrong by a factor of four. In conclusion, numerical modeling of MHD wave propagation is an essential tool for interpreting the effects of sunspots on seismic waveforms.
 Publication:

Astronomy and Astrophysics
 Pub Date:
 October 2013
 DOI:
 10.1051/00046361/201321485
 arXiv:
 arXiv:1303.6307
 Bibcode:
 2013A&A...558A.130S
 Keywords:

 Sun: helioseismology;
 sunspots;
 Astrophysics  Solar and Stellar Astrophysics
 EPrint:
 5 pages, 3 figures: submitted to A&