Large-scale horizontal flows in the solar photosphere IV. On the vertical structure of large-scale horizontal flows |
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| Authors: | M Švanda M Klvaňa M Sobotka AG Kosovichev TL Duvall |
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| Institution: | 1. Astronomical Institute (v.v.i.), Academy of Sciences of the Czech Republic, Fri?ova 298, CZ-251 65 Ond?ejov, Czech Republic;2. Astronomical Institute, Faculty of Mathematics and Physics, Charles University, V Hole?ovi?kách 2, CZ-180 00 Prague 8, Czech Republic;3. W.W. Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA 94305, USA;4. Solar Physics Laboratory, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA |
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| Abstract: | In the recent papers, we introduced a method utilised to measure the flow field. The method is based on the tracking of supergranular structures. We did not precisely know, whether its results represent the flow field in the photosphere or in some subphotospheric layers. In this paper, in combination with helioseismic data, we are able to estimate the depths in the solar convection envelope, where the detected large-scale flow field is well represented by the surface measurements. We got a clear answer to question what kind of structures we track in full-disc Dopplergrams. It seems that in the quiet Sun regions the supergranular structures are tracked, while in the regions with the magnetic field the structures of the magnetic field are dominant. This observation seems obvious, because the nature of Doppler structures is different in the magnetic regions and in the quiet Sun. We show that the large-scale flow detected by our method represents the motion of plasma in layers down to ～10 Mm. The supergranules may therefore be treated as the objects carried by the underlying large-scale velocity field. |
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