High-resolution helioseismology

Details High-resolution helioseismology High-resolution helioseismology

Jun 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985esasp.235..199h&link_type=abstract

In ESA Future Missions in Solar, Heliospheric and Space Plasma Physics p 199-208 (SEE N86-27330 18-12)

Astronomy and Astrophysics

Astronomy

105

Helioseismology, Soho Mission, Solar Oscillations, Solar Physics, Solar Interior, Solar Observatories, Solar Spectra, Spaceborne Astronomy, Spectral Resolution

Scientific paper

The basic method of helioseismology, considerations important in designing an instrument to obtain the required observations, the status of observational techniques, and results and advantages of space observations are reviewed. High resolution of solar interior conditions in radius, latitude, longitude, and time requires observations of as many different modes of oscillation as possible. Such observations can be made by measuring oscillations of brightness or the Doppler shift of suitable spectrum lines. To observe the maximum number of different modes requires angular resolution of 2 arc sec over the entire disk and time resolution of 100 sec for a duration of months. However, much can be learned with less highly resolved images. Ground based observations are limited by atmospheric blurring and by diurnal sampling distortions. By avoiding these problems the SOHO mission offers an excellent opportunity for a major advance in understanding of the solar interior.

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