Publikationsdatum:
2011-08-24
Beschreibung:
Due to the rotation of the sun the solar corona can be observed under different directions at different times. Using methods of computer tomography the three-dimensional structure of the emissivity of the solar corona can be reconstructed. We discuss the feasibility of this method for stationary and for non-stationary corona and also for incomplete and finite resolution data. As example we present reconstructions based on YOHKOH-images, and we compare the results with ground-based optical corona observations. Structures are interpreted in terms of the solar magnetic field topology.
Schlagwort(e):
Solar Physics
Materialart:
International Solar Wind 8 Conference; 68; NASA-CR-199940
Format:
text
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