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Fine Structure and Dynamics of the Inner Corona

  • G.E. Brueckner (a1), J.D.F. Bartoe (a1) and M.E. VanHoosier (a1)

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High spectral (0,05 Å) and spatial (⋍ 1000 km) resolution spectra of the Fe XII line 1349.4 Å reveal the existence of coronal fine structures in the quiet sun against the solar disk. These coronal bright elements have an average size of 2000-3000 km; their column density can be 3 x 1017 cm –2 . In the quiet sun, outward streaming velocities of 10-15 km sec –1 can be measured by means of the Doppler effect. The total kinetic and thermal energy of the outstreaming gas can be estimated to be larger than 1 x 10 5 ergs cm –2 sec –1, enough to account for the heating of the corona and the losses of the solar wind. At the outer limb (cos θ ⋍0.1) line profiles show a strong blue asymmetry, which could be caused by expanding material in a piston-driven shock, whereby the opaque, cool piston causes the asymmetry of the line profile.

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Fine Structure and Dynamics of the Inner Corona

  • G.E. Brueckner (a1), J.D.F. Bartoe (a1) and M.E. VanHoosier (a1)

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