Using data from observing seasons 1977 through 1984, an analysis of the low l, high n p-mode solar spectra is made with a 0.9 μHz resolution. Frequencies and amplitudes of modes of l < 3 and 11 < n < 33 are determined for each observing season. No clear variation of the frequencies at the 1 μHz level is found and the amplitudes remain constant to ˜ 20%. The frequency spacings between different modes are compared over the solar cycle, as are the constants in Tassoul's asymptotic formula evaluated for each season: no conclusive variations are found.