Seismic Holography of the Deep Solar Interior

Details Seismic Holography of the Deep Solar Interior Seismic Holography of the Deep Solar Interior

May 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000spd....31.0503l&link_type=abstract

American Astronomical Society, SPD Meeting #31, #05.03; Bulletin of the American Astronomical Society, Vol. 32, p.836

Astronomy and Astrophysics

Astronomy

Scientific paper

The first images of magnetic regions on the far solar surface were recently secured by applying seismic holography to five-minute oscillations with spherical harmonic degrees roughly in the range 20 to 40 in SOHO-MDI observations. These waves penetrate up to half way to the sun's center, and can therefore sample the base of the convection zone with a resolution similar to that of the aforementioned far-side images, approximately 10o in longitude at the solar equator. However, by far the best seismic diagnostics are invariably offered by the highest possible frequencies, 6 mHz and above, if possible. Because these waves are efficiently absorbed by the solar surface, helioseismic observations that can compare the far side of the sun with earth-based observations of the near side are needed for coherent phase-sensitive imaging of the deep solar interior. Coordinated near- and far-side seismic observations of the sun at frequencies in the range 6--7 mHz would allow us to examine the thermal and Doppler profile of the solar core with a resolution of 75 Mm. This presentation is based on research supported by grants NAG5-7236 from NASA and AST-9528249 from NSF, and by a contract, PY-0184, with Stanford University.

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