Coronal Polar Plumes.
Abstract
The autocorrelations and frequency spectra of the radiance of the polar corona observed during the three eclipses of the last sunspot minimum are examined. It is found that the width of polar plumes is 3.4X 10~ km, in agreement with earlier determinations, and that only marginal periodicity in the spacing of plumes is present. Statistical data supporting a connection between polar plume and polar faculae, bright K3 facula, and supergranulation cells are discussed. Our analysis shows that the observed properties of plumes are consistent with the hypothesis that these features are the result of the increased flux of material into the corona from the small-scale magnetic field concentrations which are centered on the chromospheric rosette. At sunspot minimum only a small fraction of the polar rosettes possess polar plumes while at sunspot maximum and at low latitudes it appears that every rosette supports a plume.
Related Papers
- → Energy budget in coronal holes(1973)58 cited
- → Role of Closed Magnetic Fields in Solar Wind Flow(2004)46 cited
- → Extension of coronal structure into interplanetary space(1997)59 cited
- → Coronal Hole Boundaries and their Interactions with Adjacent Regions(1999)17 cited
- The solar atmosphere and the structure of active regions(1974)