The detection and measurement of solar g-modes is of significant importance in the study of the internal structure of the Sun. The g-mode signal in intensity is predicted to peak very close to the solar limb (T. Toutain, private communication). We are developing a technique which differences the signal in a narrow annulus very close to the limb from the signal in an adjacent (interior) annulus in order to remove the solar background ``noise'' signal and thus enhance the probability of detecting g-modes. Here we present our preliminary results.
New Eyes to See Inside the Sun and Stars
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