Periodic and non-periodic phenomena in a sunspot region

• Published in: Solar physics 1996-08, Vol.167 (1-2), p.79-94
• Main Authors: Tsiropoula, G., Alissandrakis, C. E., Dialetis, D., Mein, P.
• Format: Article
• Language: English
• ISSN: 0038-0938; 1573-093X
• DOI: 10.1007/BF00146329

We have studied running penumbral waves, the homogeneous Evershed effect, and the spatial relation between intensity and Doppler velocity penumbral features of a chromospheric sunspot. The observations were obtained with the multichannel subtractive double-pass spectrograph (MSDP) operating in H alpha at the Vacuum Tower Telescope (VTT) installed at Tenerife (Canary Islands). We derived intensity and Doppler velocity maps at H alpha plus or minus 0.3 A over a two-dimensional field of view. We have computed the components of the velocity vector (radial, azimuthal, vertical) as a function of distance from the center of the spot under the assumption of axial symmetry. The results show the well-known, from previous observations, general large-scale characteristics of the chromospheric Evershed flow. Our measurements show that the axes along the discrete structures, where the Evershed flow is confined, are not spatially related to the axes along H alpha plus or minus 0.3 A intensity features, and we suggest that either the flow is confined in flow channels or that it takes place along sheared magnetic field lines. We also detected, for the first time in velocity images, running penumbral waves, which started in the outer 0.3 of the umbral radius and propagated through the penumbra with propagation velocities 13-24 km s super(-) super(1) . The propagation velocity, as well as the velocity amplitude, is greater for the waves closer to the center of the spot and diminishes as one moves outward.