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. To enhance the probability of detecting g-modes, we have tried to reduce the solar background ``noise'' signal by differencing the signal in a narrow annulus at the solar limb from the signal in an adjacent (interior) annulus. We will present some preliminary results from a study of Ca K-line intensity observations obtained at the South Pole during the austral summer of 1995/95.
AAS/Solar Physics Division Meeting #28
- Pub Date:
- May 1997