Probing Deep Structure of the Sun by Time-Distance Helioseismology

Details Probing Deep Structure of the Sun by Time-Distance Helioseismology Probing Deep Structure of the Sun by Time-Distance Helioseismology

Dec 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agufmsh11b0710b&link_type=abstract

American Geophysical Union, Fall Meeting 2001, abstract #SH11B-0710

Computer Science

Sound

7522 Helioseismology, 7524 Magnetic Fields, 7544 Stellar Interiors And Dynamo Theory

Scientific paper

Time-distance helioseismology is a method for inferring sound-speed perturbations and flow velocities by measuring the travel times for acoustic wave packets as they move between points on the solar surface through the solar interior. It has been successfully applied to infer structures and flows in the upper convection zone. However, probing the deep convection zone and, in particular, the tachocline region at the bottom of the convection zone where the solar dynamo is believed to be operating is quite challenging. Using the solar oscillation data from SOHO/MDI we have attempted to detect deep structures in a low-latitude band of the convection zone. For inversion of the travel-time measurements we used the theoretical sensitivity, in the first Born approximation, of travel times to sound speed inhomogeneities in the solar convection zone. We have obtained synoptic sound-speed maps for two solar rotations in 2000. The results show resolved structures in the lower convection zone. We compare the sound-speed maps with surface magnetic field synoptic maps and discuss possible relations between the deep structures and the surface field.

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