AbstractThe pattern of emission coronal green line brightness (Fe XIV 530.3nm) has been used as a tracer to determine differential rotation of the solar corona. Detailed knowledge of the solar rotation seems to be crucial for understanding of the magnetic field generation within the sun’s convection zone and for explanation of the cyclic evolution of solar activity. Spectral variation analysis (SVAN) was applied to our own database of the coronal green line brightness (CGLB) covering almost six solar cycles (1939–2001). It was found that the period of rotation increases from 27 days at the solar equator to a little more than 29 days within the latitudes ±40°, displaying in this way much less pronounced differential rotation than the majority of the photospheric phenomena do. At the higher latitudes the rotation period changes very slowly and its value of about 29 days remains up to the polar regions. An assumption on the presence of two modes in the coronal rotation seems to be feasible to explain the results obtained. Comparison of the found results with the latest helioseismic measurements is discussed.
Two modes of rotation in the solar corona
Advances in Space Research ; 38 , 5 ; 906-911
2006-03-28
6 pages
Aufsatz (Zeitschrift)
Elektronische Ressource
Englisch
Two modes of rotation in the solar corona
British Library Conference Proceedings | 2006
|Two modes of rotation in the solar corona
Online Contents | 2006
|TEMPORAL VARIATIONS OF THE SOLAR CORONA ROTATION
British Library Conference Proceedings | 2005
|Rotation of the Extended Solar Corona from SOHO/UVCS Observations
British Library Conference Proceedings | 2006
|Solar Corona as Indicator of Differential Rotation of Subphotospheric Layers
Online Contents | 2019
|