A way to examine rotational splittings without explicit foward or inverse computations

Details A way to examine rotational splittings without explicit foward or inverse computations A way to examine rotational splittings without explicit foward or inverse computations

Dec 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988esasp.286..137m&link_type=abstract

In ESA, Seismology of the Sun and Sun-Like Stars p 137-140 (SEE N89-25819 19-92)

Computer Science

Numerical Analysis

4

Angular Velocity, Solar Activity Effects, Solar Interior, Solar Oscillations, Solar Rotation, Convection, Depth, Latitude, Numerical Analysis, Velocity Distribution

Scientific paper

Simple techniques for extracting information about the Sun's internal rotation from the observed frequency splittings of solar acoustic oscillations are derived. The techniques do not require any formal forward or inverse computations and yet are signicantly revealing about the radial and latitudinal variations of solar angular velocity reflected by the data. Simple linear combinations of the familiar rotational splitting coefficients a1(L), a3(L), a5(L), where L = l(l+1) and l is the angular degree of an oscillation mode, allow one to gain an impression of how any chosen colatitudinal average of the angular velocity varies with depth, or of the radial variation of angular velocity at any particular colatitude. The techniques are easy to apply and are illustrated using the data of Brown and Morrow. The methods reveal a lack of a substantial radial gradient of angular velocity in the convection zone, and a reversal in the sign of the radial gradient of angular velocity at 30 deg latitude at depths near the base of the convection zone. When subject to more detailed forward and inverse analysis, these data also suggest such characteristics of the solar internal angular velocity. This lends credence to the methods described.

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