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A Dynamo Confinement Scenario for the Solar Tachocline and Its Implications for Spin-down in the Radiative Spreading Regime

  • Authors: Loren I. Matilsky, Lydia Korre, Nicholas H. Brummell

Loren I. Matilsky et al 2026 The Astrophysical Journal 1005 .

  • Provider: AAS Journals

Caption: Figure 11.

Time–latitude diagrams over the interval t = (27500, 52500) of ﹩{\rm{Re}}({B}_{\theta }^{1})﹩ in the upper RZ (﹩{r}^{\ast }﹩/R = 0.692) and the corresponding truncated horizontally averaged power spectra in frequency ﹩{\left\langle {\left|{B}_{\theta }^{1\omega }\right|}^{2}\right\rangle }_{{\rm{sph}}}﹩ for (a)–(b) Case M3, (c)–(d) Case M4, and (e)–(f) Case M6. The full time series t = (0, trun) was used to obtain the frequency spectra and a Hanning window function was employed to reduce high-frequency noise. For Cases M3, M4, and M6, respectively, the frequency resolution (the width of the bars) is 1/trun = 6.06 × 10−5, 2.08 × 10−4, and 1.35 × 10−4 and the Nyquist frequencies are 1/(2Δt) = 0.151, 0.247, and 0.147, where Δt is the average sampling cadence.

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