Abstract
A large equatorial coronal streamer observed in the outer corona (3R ⊙) grew in brightness and size during successive limb passages between October 6, 1973 and January 10, 1974 (solar rotations 1606–1611). Unlike previous studies of streamers and their photospheric associations, no definite surface feature could be identified in the present case. This suggests that the streamer is associated with the large scale photospheric magnetic field. Comparison of the streamer growth with observed underlying photospheric magnetic flux changes indicated that as the streamer increased in brightness, areal extent, and density, the photospheric magnetic flux decreased. Three possible explanations for the streamer's growth are presented; the conceptually simplest being that the decrease in photospheric field results in an opening of the flux tubes under the streamer which permits an increased mass flux through the streamer.
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The National Center for Atmospheric Research is sponsored by the National Science Foundation.
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Poland, A.I., Macqueen, R.M. The evolution of a coronal streamer and the photospheric magnetic field. Sol Phys 71, 361–379 (1981). https://doi.org/10.1007/BF00167558
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DOI: https://doi.org/10.1007/BF00167558