Plasma flows and sound-speed perturbations in the average supergranule

Abstract

Context. Supergranules create a peak in the spatial spectrum of photospheric velocity features. Even though they have some properties of convection cells, their origin is still being debated in the literature. The time–distance helioseismology constitutes a method that is suitable for investigating the deep structure of supergranules. Aims. Our aim is to construct the model of the flows in the average supergranular cell using fully consistent time–distance inverse methodology. Methods. We used the Multi-Channel Subtractive Optimally Localised Averaging inversion method with regularisation of the cross-talk. We combined the difference and the mean travel-time averaging geometries. We applied this methodology to travel-time maps averaged over more than 104 individual supergranular cells. These cells were detected automatically in travel-time maps computed for 64 quiet days around the disc centre. The ensemble averaging method allows us to significantly improve the signal-to-noise ratio and to obtain a clear picture of the flows in the average supergranule. Results. We found near-surface divergent horizontal flows which quickly and monotonously weakened with depth; they became particularly weak at the depth of about 7 Mm, where they even apparently switched sign. The amplitude of the ‘reversed’ flow was comparable to the background flows. The inverted vertical flows and sound-speed perturbations were spoiled by unknown systematic errors. To learn about the vertical component, we integrated the continuity equation from the surface. The derived estimates of the vertical flow depicted a sub-surface increase from about 5 m s−1 at the surface to about 35 m s−1 at the depth of about 3 Mm followed by a monotonous decrease to greater depths. The vertical flow remained positive (an upflow) and became indistinguishable from the background at the depth of about 15 Mm. We further detected a systematic flow in the longitudinal direction. The course of this systematic flow with depth agrees well with the model of the solar rotation in the sub-surface layers.

Imaging the Sun's near-surface flows using mode-coupling analysis

“…But, to recapitulate, a host of factors described above can skew the amplitudes for divergence flows owing to the multi-step process involved in obtaining them. For example, there has been a history (see, e.g., De Rosa et al 2000;Sekii et al 2007;Zhao et al 2007;Langfellner et al 2018;Böning et al 2020;Korda & Švanda 2021) of using travel-time difference as only a proxy for horizontal divergence. However, Langfellner et al (2015), Birch et al (2016) and Birch et al (2019) use empirically determined conversion factors to align flow amplitudes from travel-time measurements with those of LCT, while acknowledging that LCT underestimates magnitudes (see Verma et al 2013;Löptien et al 2016).…”