We explore the use of the flux difference between the lines Fe 15250 Å and Fe 15247 Å as a technique to measure photospheric magnetic fields in late-type stars. The technique developed takes into account all the LTE physics of the problem, assuming a radial and homogeneous magnetic field distribution over the stellar surface. Some test calculations

The characteristics of the three different principal data sets that have been extensively analyzed in a search for g-modes (Tenerife, ACRIM, and Stanford) are reviewed, and the results claimed from the analysis are examined. It is noted that discrepancies betwen observers suggest that, though they have probably been detected, the solar g-modes have

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Mathematical formulas derived from solar p-mode frequencies not only accurately reproduce observed frequencies, but extrapolate them to limits beyond current observations. Over 1500 solar p-mode frequencies have thus far been measured for different mode degrees and numbers. Attention is here given to the Tassoul first- and second-order asymptotic

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