Abstract
During a balloon flight in France on September 13, 1971, at altitude 32 000 m, the solar corona was cinematographed from 2 to 5R ⊙ during 5 hr, with an externally occulted coronagraph.
Motions in coronal features, when they occur, exhibit deformations of structures with velocities not exceeding a few 10 km s−1; several streamers were often involved simultaneously; these variations are compatible with magnetic changes or sudden reorganizations of lines of forces.
Intensity and polarization measurements give the electron density with height in the quiet corona above the equator. Electron density gradient for one of the streamers gives a temperature of 1.6 × 106 K and comparisons with the on-board Apollo 16 coronal observation of 31 July, 1971 are compatible with the extension of this temperature up to 25 R bd.
Three-dimensional structures and localizations of the streamers are deduced from combined photometry, polarimetry and ground-based K coronametry. Three of the four coronal streamers analysed have their axis bent with height towards the direction of the solar rotation, as if the upper corona has a rotation slightly faster than the chromosphere.
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Dollfus, A., Mouradian, Z. Electrons in the solar corona. Sol Phys 70, 3–24 (1981). https://doi.org/10.1007/BF00154390
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DOI: https://doi.org/10.1007/BF00154390