Deeply penetrating banded zonal flows in the solar convection zone

Details Deeply penetrating banded zonal flows in the solar convection zone Deeply penetrating banded zonal flows in the solar convection zone

2000-03-08

arxiv.org/abs/astro-ph/0003121v1

Astronomy and Astrophysics

Astrophysics

4 pages, 4 figures To be published in ApJ Letters (accepted 3/3/2000)

Scientific paper

10.1086/312623

Helioseismic observations have detected small temporal variations of the rotation rate below the solar surface corresponding to the so-called `torsional oscillations' known from Doppler measurements of the surface. These appear as bands of slower and faster than average rotation moving equatorward. Here we establish, using complementary helioseismic observations over four years from the GONG network and from the MDI instrument on board SOHO, that the banded flows are not merely a near-surface phenomenon: rather they extend downward at least 60 Mm (some 8% of the total solar radius) and thus are evident over a significant fraction of the nearly 200 Mm depth of the solar convection zone.

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