Previous
abstract 
Next
abstract
Measurements of the rotation rate in the deep solar interior using helioseismology have given inconsistent results, presumably due to problems with the algorithms used for the analysis of spatially unresolved observations of the oscillations. Here we present a measurement of the rotation rate in the interior of the Sun based on observations with a new instrument called LOWL. Unlike earlier instruments this instrument allows the observation of oscillations with degrees from 0 to $\approx 80$. In particular it is able to make spatially resolved observations of low degree modes, thereby making it possible to spatially separate the different modes within a given multiplet. This reduces the potential for systematic errors compared to observations using integrated sunlight. We have used observations of the frequency splittings of modes with degrees from 1 to 80 to infer the rotation rate in the solar interior down to $\approx 0.2 R_{\sun}$ with some radial resolution and without excessive errors. Over part of the range we have also been able to estimate the latitudinal variation of the rotation rate. This measurement provides strong constraints on the theories of solar and stellar angular momentum transport.
