Sunspot's magnetic and velocity field within the convective network

Details Sunspot's magnetic and velocity field within the convective network Sunspot's magnetic and velocity field within the convective network

Oct 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002esasp.505..365b&link_type=abstract

In: SOLMAG 2002. Proceedings of the Magnetic Coupling of the Solar Atmosphere Euroconference and IAU Colloquium 188, 11 - 15 Jun

Physics

Sunspots, Magnetic Fields

Scientific paper

From 81 sets of photoelectric measurements of the line-of-sight velocity component in the Evershed effect of a regular sunspot, made during 8 days with electronically enhanced sensitivity, we have estimated the main characteristics of the Evershed flow in the measured spot: the motion in the center of the spot is probably slightly upwards, it is then almost horizontal and finally, in its peripheral part, it is possibly slightly inclined below the solar surface. We draw attention to the existence of regular secondary structures of the Evershed effect, surrounding the primary effect and to the mutual unity of their motions. Together they form one physical entity, which fits the structure of the motion field of the surrounding magnetised photosphere well. But the whole active region's motion field represents the same kind of disturbance of the semiregular motion patterns of the quiet photosphere, in which the positive Doppler motion elements are considerably diluted and the negative elements strongly concentrated and organised. We also demonstrate the relationship of the distribution of the active region's magnetic and negative velocity fields with the emission patterns of the K3 Ca II and of the positive motion elements with the dark interiors of the same K3 Ca II supergranules.

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