Astronomy and Astrophysics – Astrophysics
Scientific paper
Dec 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsh53b..04a&link_type=abstract
American Geophysical Union, Fall Meeting 2010, abstract #SH53B-04
Astronomy and Astrophysics
Astrophysics
[7509] Solar Physics, Astrophysics, And Astronomy / Corona, [7522] Solar Physics, Astrophysics, And Astronomy / Helioseismology
Scientific paper
Howe et al. (2009) demonstrate that solar activity appears to move towards the equator somewhat parallel to the latitude motion of torsional oscillation flows. However, Snodgrass (1987) had previously suggested that the regions between the fast and slow torsional oscillation flows represent zones where magnetic field is concentrated, which results in the formation of activity. In an attempt to test this suggestion, Altrock et al. (2008) compared the location of bright Fe XIV coronal regions to the latitude derivative of torsional oscillation frequencies and found that the bright regions occurred over regions where the latitude derivative was at its lowest (negative) value; i.e., between the fast and slow streams, thus verifying Snodgrass' suggestion. This paper extends and verifies the results of Altrock et al., that SOLAR ACTIVITY OCCURS OVER THE ``SHEAR'' ZONE BETWEEN FAST AND SLOW TORSIONAL OSCILLATION FLOWS. References: Howe, R., et al., ApJ Letters 701, L87, 2009; Snodgrass, H., ApJ 316, L91, 1987; Altrock, R., et al., ASPCS 363, 335, 2008. Thanks to R. Howe and R. Ulrich for providing their torsional oscillation data. Fe XIV coronal bright regions (shading) and MWO torsional oscillation latitude derivative (contours) from 1982 to 2007.
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