Long-Term Variation of the Rotation of the Solar Corona

Details Long-Term Variation of the Rotation of the Solar Corona Long-Term Variation of the Rotation of the Solar Corona

Jan 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002mwoc.conf..337a&link_type=abstract

Multi-Wavelength Observations of Coronal Structure and Dynamics -- Yohkoh 10th Anniversary Meeting. Proceedings of the conferenc

Astronomy and Astrophysics

Astrophysics

Scientific paper

Synoptic photoelectric observations of the coronal Fe XIV and Fe X emission lines at 530.3 nm and 637.4 nm, respectively, are analyzed to study the rotational behavior of the solar corona as a function of latitude, height and time. The data used are measurements made with the Sacramento Peak 40-cm coronagraph and Emission-Line Coronal Photometer of the intensity of these lines observed at 1.15 to 1.45 solar radii (Ro) between 1973 (1984 for Fe X) and 2000. An earlier similar temporal-correlation analysis of the Fe XIV data at 1.15 Ro over only one 11-year solar activity cycle (Sime, Fisher and Altrock 1989, Astrophys. J. 336, 454) found suggestions of solar-cycle variations in the differential-rotation and latitude-averaged-rotation patterns that combined the effects of large-scale patterns seen in the white-light corona and smaller-scale patterns seen in chromospheric and photospheric rotation. These results will be tested over the longer epoch now available. In addition, the new 1.15 Ro Fe XIV results will be compared with those at greater heights and with results from the Fe X line and radio frequencies (Vats et al. 2001, Astrophys. J., 548, L87) to form a global picture of solar rotation throughout the corona and over more than two solar cycles.

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