Fig. B.1.
Kinetic energy density (ρr2(ξr(r)2 + l(l + 1)ξh(r)2) [g cm]) as a function of fractional solar radius r/R⊙ for modes with degree lp = lg = 1. The radial orders and frequencies of the modes are given in each panel. Compare to Fig. 1 from Provost et al. (2000). We note that the mode frequencies are slightly different compared to Provost et al. (2000) due to slight differences in the solar model.
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