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Evolution of coronal helmets during the ascending phase of solar cycle 20

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Abstract

The principal polar-crown coronal helmet structures were selected from nearly three years (May, 1965–January, 1968) of K-coronameter observations made at Haleakala and Mauna Loa, Hawaii. Six isolated and long-lived helmet systems were found at latitudes of 45° and above. Their developments are compared with underlying chromospheric and photospheric activity and a simple phenomenological model is presented showing that a coronal system is formed over an active region. Thereafter the center of gravity of the system gradually drifts poleward with the trailing unipolar magnetic region (UMR), and it becomes a high latitude coronal helmet, arched over a polar crown filament.

By comparison of these coronal helmets with observations of the outer corona (to circa 4 R ) made at solar eclipse, lunar sunset, and with balloon and rocket-borne externally occulted corona-graphs, it appears that ground-based K-coronameter measurements to a distance of 1.5–2.0 R are sufficient to detect the coronal streamers.

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The National Center for Atmospheric Research is sponsored by the National Science Foundation.

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Hansen, S.F., Hansen, R.T. & Garcia, C.J. Evolution of coronal helmets during the ascending phase of solar cycle 20. Sol Phys 26, 202–224 (1972). https://doi.org/10.1007/BF00155120

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  • DOI: https://doi.org/10.1007/BF00155120

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