Local Helioseismology of Magnetoconvective Sunspot Simulations and the Reliability of Standard Inversion Methods

Details Local Helioseismology of Magnetoconvective Sunspot Simulations and the Reliability of Standard Inversion Methods Local Helioseismology of Magnetoconvective Sunspot Simulations and the Reliability of Standard Inversion Methods

May 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011spd....42.1607b&link_type=abstract

American Astronomical Society, SPD meeting #42, #16.07; Bulletin of the American Astronomical Society, Vol. 43, 2011

Statistics

Methodology

Scientific paper

Controversy exists in the interpretation and modeling of helioseismic signals in and around magnetic regions like sunspots. We show the results of applying local helioseismic inversions to travel-time shift measurements from realistic magnetoconvective sunspot simulations. We compare travel-time maps made from several simulations, using different measurements (helioseismic holography and center-annulus time distance helioseismology), and made on real sunspots observed with the HMI instrument onboard the Solar Dynamics Observatory. We find remarkable similarities in the travel-time perturbations measured between: 1) simulations extending both 8 and 16 Mm deep, 2) the methodology (holography or time-distance) applied, and 3) the simulated and real sunspots. The application of RLS inversions, using Born approximation kernels, to narrow frequency-band travel-time shifts from the simulations demonstrates that standard methods fail to reliably reproduce the true wave speed structure. These findings emphasize the need for new methods for inferring the subsurface structure of active regions. Artificial Dopplergrams from our simulations are available to the community at www.hao.ucar.edu under "Data" and "Sunspot Models." This work is supported by NASA under the SDO Science Center project (contract NNH09CE41C).

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