Solar radiation models and the a1, a3 and a5 splitting coefficients for solar acoustic oscillations

Details Solar radiation models and the a1, a3 and a5 splitting coefficients for solar acoustic oscillations Solar radiation models and the a1, a3 and a5 splitting coefficients for solar acoustic oscillations

Dec 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988esasp.286...91m&link_type=abstract

In ESA, Seismology of the Sun and Sun-Like Stars p 91-98 (SEE N89-25819 19-92)

Computer Science

5

Angular Velocity, Solar Activity Effects, Solar Oscillations, Solar Rotation, Helioseismology, Kernel Functions, Stellar Models

Scientific paper

A forward analysis of the rotational frequency splittings of solar p-modes measured by Brown and Morrow (1987) was done to obtain information on the variation of the Sun's angular velocity with depth and co-latitude. This approach entails computing frequency splittings for chosen models of the solar rotation and comparing them to the observed splittings. It is called a forward method to contrast it with inversion techniques, which use the measured frequency splittings directly to produce a single function for the angular velocity. An advantage of the forward approach is that it allows one to develop intuition about the sensitivities of the splitting coefficients (a1, a3, and a5) to various changes in the nature and magnitude of the angular velocity. The results of the analysis conducted in Morrow (these proceedings) give the impression that models with surface rotation throughout the convection zone are more promising than models with angular velocity constant on cylinders. The more formal approach used here substantiates this impression, and can consider the splittings from a series of more elaborate models for the solar rotation.

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